quarks and cosmos book of abstracts - my web page

Book of Abstracts 1

7th International Workshop on Astronomy andRelativistic Astrophysics (IWARA 2016): Quarks

and Cosmos

Book of Abstracts

Heuristic Approach on Anomalous Apsidal Precession of PlanetsAbraao Jesse Capistrano de Souza*, Joice A. M. Penagos,

and Manuel S. AlarconUniversidade Federal da Integracao Latino Americana (UNILA)

Foz do Iguacu, Brazil

Abstract: We investigate the anomalous planets precession in the nearly-newtoniangravitational regime. Using a non-standard expression for the perihelion ad-vance from the Weyl conformastatic vacuum solution as a model, we describethe anomalous movement in planets precession as compared to different obser-vational data from Ephemerides of the Planets and the Moon (EPM2008 andEPM2011) and the Planetary and Lunar Ephemeris (INPOP10a). As a firstapproximation, we use heuristic methodology obtaining a very close results toobservations. (email*: [email protected])

Excitation Wave Magnetohydrodynamic (MHD) by GravitationalWaves Produced by Binary of the Neutron Stars

Adam Smith Gontijo Brito de Assis* and Oswaldo D. MirandaInstituto Nacional de Pesquisas Espaciais (INPE)

Sao Jose dos Campos, Brazil

Abstract: Relativistic magnetohydrodynamics (MHD) plays an important rolein high-energy astrophysics. In events like the γ-Ray Bursts (GRBs), relativisticplasmas and strong magnetic fields are believed to be involved in the extractionof energy from the central objects. These plasmas, according to the fireballmodel, consisting of electron-positron pair, radiation and baryonic matter. Thelatter acquires the greater part of the explosion energy, reaching Lorentz factorson the order 102 − 103. The most promising progenitor to generate a GRBshort (less than 2 sec) is merger binary systems (NS-NS and NS-BH). Suchsistems produce significant amount of gravitational waves (GW) and are can-didates to be detected by ground detectors (eg, Advanced LIGO, in the range10Hz − 1kHz). We review the excitation mechanism of MHD wave modes ina strongly magnetized plasma surrounding the source of gravitational radiationbefore the merger of neutron stars; assuming that the gravitational wave is weak,we linearize the GR-MHD equations and find the analytical solutions. In par-ticular, it is shown that the magnetosonic modes are coupled to the polarization+ gravitational wave and the Alfven mode, polarization ×. Such a coupling fora NSs binary system near merger, was studied at work Moortgat (2006). The

2 IWARA 2016 - Gramado, Brazil - 9 - 13 October 2016

author found that the higher amount of gravitational wave emission occurs inthe frequency ωg ∼ 1kHz and he calculated the energy deposited in the plasmathrough interaction of the GW polarizations with MHD wave modes. We con-sider the formalism adopted by Moortgat (2006) to derive the equations thatdescribe the interaction, but now considering spiral phase from a minimum fre-quency (ωg ∼ 300Hz) for effective interaction to the frequency of the last stableorbit system (ωg ∼ 1.5kHz). In particular, we show that the amount of energyGW dissipated into the plasma and associated with the Alfvn mode duringspiralphase, can be as high as 1040J. (email*: [email protected])

Do Massive Neutron Stars end as Invisiable Dark Energy Objects?Ahmad A. Hujeirat

Interdisziplinares Zentrum fur Wissenschaft Rechnen (IWR)der Universitat Heidelberg

Heidelberg, Germany

Abstract: Astronomical observations reveal a gap in the mass spectrum of rel-ativistic objects: neither black holes nor neutron stars having masses in therange of 2−5MSun have ever been observed. Based on the solution of the TOVequation modified to include a universal scalar field H, we argue that all moder-ate and massive neutron stars should end invisible dark energy objects (DEOs).Triggered by theH−baryonic matter interaction, a phase transition from normalcompressible nuclear matter into an incompressible quark-superfluid is shownto occur at roughly 3 times the nuclear density. At the transition front, thescalar field is set to inject energy at the maximum possible rate via a non-localinteraction potential Vϕ = a0r

2+ b0. This energy creates a global confining bag,inside which a sea of freely moving quarks is formed in line with the asymptoticfreedom of quantum chromodynamics. The transition front, rf , creeps frominside-to-outside to reach the surface of the object on the scale of Gyrs or evenshorter, depending on its initial compactness. Having rf reached R⋆, then thetotal injected dark energy via Vϕ turns NSs into invisible DEOs. While this mayprovide an explanation for the absence of stellar BHs with MBH ≤ 5MSun andNSs with MNS ≥ 2MSun, it also suggests that DEOs might have hidden connec-tion to dark matter and dark energy in cosmology (email: [email protected])

LIGO and the First DiscoveriesAlbert Lazzarini

LIGO Laboratory, California Institute of TechnologyPasadena, EUA

Abstract: Advanced LIGO became operational in the late summer of 2015.Shortly after it reached stable operational sensitivity it detected coincidentsignals at the two LIGO observatories from the coalescence and merger of apair of massive black holes. I will discuss how LIGO operates as a gravita-tional wave detector and then provide details of our first discoveries. (email:[email protected])

Book of Abstracts 3

New Tetrads in Riemannian Geometry and New Ensuing Resultsin Group Theory, Gauge Theory and Fundamental Physics, in

Particle Physics, General Relativity and AstrophysicsAlcides Garat

Universidad de la Republica (UdelaR)Montevideo, Uruguay

Abstract: A new technique is presented in order to build tetrads in four-dimensional Lorentzian spacetimes. These tetrads have special useful propertiesin general relativity, astrophysics and also particle physics. A new fundamentalresult is proved in group theory using these tetrads. The group SO(2) (spatialrotations) is isomorphic to the group SO(1;1) (boosts) plus two kinds of discretetransformations. One of them is not Lorentzian. That is, a compact group isisomorphic to a non-compact group plus two different kinds of discrete transfor-mations (A. Garat, Tetrads in geometrodynamics, J. Math. Phys. 46, 102502(2005) and (A. Garat, Tetrads in Yang-Mills geometrodynamics, Gravitationand Cosmology, (2014) Vol. 20 No. 1, pp. 116-126. Pleiades Publishing Ltd.)The electromagnetic local gauge group is proved to be isomorphic to the localgroup of transformations of these particular kind of tetrads. Therefore, estab-lishing a concrete link between internal and spacetime local groups of transfor-mations. These new tetrads also diagonalize the electromagnetic stress-energytensor for non-null electromagnetic fields, any stress-energy tensor, in a general,covariant and local way. These new tetrads also introduce maximum simplifi-cation in the Einstein-Maxwell differential equations, and introduce maximumsimplification in the expression of the electromagnetic field itself, in any curvedfour-dimensional Lorentzian spacetime, allowing for the identification of its de-grees of freedom in two local scalars. These tetrads introduce simplificationin spacetime evolution algorithms, specially in astrophysical situations related,for example, to neutron stars (A. Garat, Euler observers in geometrodynamics,Int. J. Geom. Meth. Mod. Phys., Vol. 11 (2014), 1450060). This new tetradcan be applied and introduce simplification in the analysis of astrophysical rel-ativistic problems where vorticity is present through the Carter-Lichnerowiczequation (A. Garat, Covariant diagonalization of the perfect fluid stress-energytensor, Int. J. Geom. Meth. Mod. Phys., Vol. 12 (2015), 1550031). (email:[email protected])

Hydrodynamics Formation of the Gamma Cephei SystemBarbara Celi Braga Camargo, Othon C. Winter,

and Dietmar W. ForytaFaculdade de Engenharia de Guaratingueta

Universidade Estadual Paulista (FEG/UNESP)Guaratingueta, Brazil

Abstract: The discovery of the exoplanets showed that many systems havegiant planets very close of the stars which orbit. These configurations were asurprise to the scientific community, as the Solar System has giant planets atlarge distances from the Sun. Jupiter, the gaseous planet closest to the Sun, itis at a distance of 5.20 AU. The Gamma Cephei binary system has your twostars very close, approximately 20 UA of distance. Besides the two stars, the


system has a planet at 2.05 UA with a mass nearby of 1.85 Jupiter masses. Inthis work, we analyzed the characteristics required in the initial stage of a diskof gas for the formation of Gamma Cephei b. The simulations are performedwith FARGO 2D (MASSET, 2000). The results and analyzes are in progressand will be presented on the meeting. (email: [email protected])

Low Energy KN Interaction in the Fock-Tani FormalismBruna Cesira Folador*, Daniel Tavares da Silva,

and Dimiter HadjimichefUniversidade Federal do Rio Grande do Sul (UFRGS)

Porto Alegre, Brazil

Abstract: The Fock-Tani formalism is a first principle method to obtain effec-tive interactions from microscopic Hamiltonians. Originally derived for meson-meson or baryon-baryon scatttering, we present the correponding equations formeson-baryon scattering. In particular we shall obtain the low energy cross-sections for the K− + p → Λ + η channel. (email*: [email protected])

Frequency Tracking Noise of b Gravitational Wave Detector NiobeCarlos Frajuca

Universidade de Sao Paulo (USP)Sao Paulo, Brazil

Abstract: This work studies the influence of the frequency tracking noise of theNiobe gravitational wave (GW) detector. The University of Western Australiaoperated the GW detector Niobe at Perth, Australia. It was a resonant-massbar detector made of niobium operating at a temperature of 5 K. It was sensitivearound the frequency of 700 Hz and had a burst sensitivity of h 7 x 10-19 witha long term operation from 1993 to early 1998. It had the lowest observednoise temperature. Using the characteristics of the detector, NIOBE shouldhad reached a much better sensitivity that the one measure. It seems that thenoise introduced in the system by the frequency tracking device was not takeninto at the time, this noise gives a value of 2.5 x 10-18 m/(Hz) -1/2, whatis the value that limited the detector sensitivity to the one measured. (email:[email protected])

The QCD Phase-diagram Obtained from NJL and Extended-NJLModels for Quark and Hadron Phases

Clebson Abati GraeffUniversidade Tecnologica Federal do Parana, Campus Pato Branco

(UTFPR-PB)Pato Branco, Brazil

Universidade Federal de Santa Catarina (UFSC)Florianopolis, Brazil

Abstract: We analyse the hadron/quark-gluon-plasma phase transition describedby the Nambu-Jona-Lasinio (NJL) model [quark phase] and the extended Nambu-Jona-Lasinio model (eNJL) [hadron phase]. While the original formulation of

Book of Abstracts 5

NJL model is not capable of describing hadronic properties due to its lack ofconfinement, it can be extended with a scalar-vector interaction so it exhibitsthis property, the so-called eNJL model. As part of this analysis, we obtainthe equations of state within the SU(2) versions of both models for for thehadron and the quark phases, and determine the binodal surface. (email: [email protected])

On Interacting Dark EnergyClement Stahl

International Center for Relativistic Astrophysics Network (ICRANet)Pescara, Roma, Italy

Abstract: We investigate a cosmological model of interacting dark matter anddark energy. This model has two extra parameters δg and δΛ which correspondsto the rate of conversion of dark matter into dark energy. We perform a χ2

fit with the supernovae IA data to constrain this new model and find that theinteracting model obtains a better χ2 than the standard cosmological model.We then explore the range of parameter of the model which gives a better χ2

than the standard cosmological model. Our conclusion is that the class of model,we investigated, provided once again a decent alternative to the ΛCDM model.(email: [email protected])

Submergence and Re-difussion of Magnetic Field PostCore-collapse

Cristian Giovanny BernalFundacao Universidade Federal de Rio Grande (FURG)

Rio Grande, Brazil

Abstract: I revisit the hyper-accretion phase, in the core-collapse supernovascenario, when a reverse shock is formed few moments after the explosion. Wefocus our study on the complex dynamics present in the system when strongaccretion allows depositing large amounts of matter onto the stellar surface andwe follow their consequences. We carry out magnetohydrodynamic numericalsimulations of the hypercritical regime, using the AMR Flash method. (email:[email protected])

Double Heavy Quark-antiquark Pair Production in Double PartonScattering Processes

Cristiano Brenner Mariotto and R. Palota da SilvaFundacao Universidade Federal de Rio Grande (FURG)

Rio Grande, Brazil

Abstract: The high gluon density in the initial state of hadronic collisions atLHC energies implies that the probability of multiple parton interactions withinone proton-proton collision increases. In particular, this motivates one to inves-tigate the importance of Double Parton Scattering (DPS) processes at the LHC.In a DPS process one can have, from one proton-proton collision, two interact-ing partons coming from each colliding hadron. In this context, the relation


between the double parton distribution functions (dPDF) and the usual partondistribution functions (PDF) is discussed, and some formulae for the DPS crosssection are compared. Our results focus on the production of different finalstates related to two heavy quark-antiquark pairs. Those include cccc, whichis called the golden channel of DPS, bbbb and ccbb. Additionally, we intend toestimate the DPS cross section for double quarkonium production, associatedproduction of quarkonium and open charm, as well as the production of multipleD and B mesons at the LHC. (email*: [email protected])

Nonlinear Walecka Model for Neutron StarsDaniel Castro Romao* and Debora Peres Menezes


Abstract: In this undergraduate work we seek to investigate the effects of dif-ferent sets of parameters and variations of the Walecka model in describing thebulk properties of a neutron star. The variations in the equation of state, appliedincrementally, are such as different proton fractions and beta stability, the ad-dition of leptons, charge neutrality and the inclusion of nonlinear terms to theLagrangian. For the star properties we use the Tolman-Oppenheimer-Volkoffequation. (email*: [email protected])

Quadrupole of a Composite Mass Optimization in Very HighSpeed Using FEM

Daniel Coppede*, Paulo Roberto Murger Nogueira,and Carlos Frajuca

Instituto Federal de Educacao, Ciencia e Tecnologia de Sao Paulo (IFSP)Sao Paulo, Brazil

Abstract: A experiment to measure the velocity of gravity is been planning. Inorder to achieve a reasonable signal in the detector, a very massive quadrupolemass is put to rotate at a very high rotation speed. In order to maximize the sig-nal, the product mass and rotation radius squared much be as higher as possible.This work test a composite mass-quadrupole geometries in Finite Element Mod-eling with the goal to maximize the signal. (email*: [email protected])

Dark Matter in a Bimetric PortalDimiter Hadjimichef

Universidade Federal do Rio Grande do Sul (UFRGS)Porto Alegre, Brazil

Abstract: One of the great mysteries in current physics is the nature of darkmatter. Originally discovered as a form of “unseen” matter that modified thedynamics of galactic clusters. Today dark matter is extensively studied in as-trophysics and in particle physics. Arguments are brought forward to considera form dark matter, manifested as a broken local dual symmetry of a bimetricspin-2 theory in the Fierz representation. (email: [email protected])

Book of Abstracts 7

Exploring the BEC-BCS Crossover in a Cold and Magnetized TwoColor QCD

Dyana Cristine Duarte*, P. G. Allen, R. L. S. Farias, Pedro H. A.Manso, Rudnei O. Ramos, and N. N. Scoccola

Universidade Federal de Santa Maria (UFSM)Santa Maria, Brazil

Abstract: There are many motivations to study the phase structure of quan-tum chromodynamics (QCD), related to investigations of the relativistic heavyion collisions, compact stars and the early universe. Moreover, the QCD phasediagram remains poorly understood, despite the many efforts dedicated to itsdescription in recent years. Further motivated by the fact that strong magneticfields may be produced in noncentral heavy-ion collisions, investigations of theeffects produced by a magnetic field in the phase diagram of strongly interactingmatter became a subject of great interest in recent years. Due to fermion signproblem, the implementation on lattice of the QCD phase diagram studies atfinite temperature and densities, then many low energy effective models, suchas quark-meson model and chiral perturbation theory are used to study thephase diagram of strongly interacting matter. It is expected that a crossoverfrom Bose-Einstein Condensation (BEC) to Bardeen-Cooper-Shriffer condensa-tion (BCS) for diquarks at finite baryon density. This crossover may happenwhen the coupling constant of the attractive interations increases, or chang-ing the charge number through the increase of the chemical potential, at smalltemperature. In this work we study the BEC-BCS crossover for a two colorNambu-Jona-Lasinio (NJL) model with diquark interactions in the presence ofan external magnetic field, devoting special attention to different regularizationschemes used in the literature. We verify the influence of this field in the phasediagrams, for both critical chemical potentials (first for BEC phase transitionand then for BEC-BCS crossover) at zero temperature. Additionally, we use amethod that makes a full separation of the finite magnetic contributions of thedivergencies, the Magnetic Field Independent Regularization (MFIR) to showthat unphysical oscillations that usually appears when using common regular-ization schemes completely disappear. (email*: [email protected])

The Pierre Auger Observatory: recent results and plannedupgrades

Edivaldo Moura SantosDepartamento de Fısica Experimental

Laboratorio do Acelerador Linear (LAL)Instituto de Fısica, Universidade de Sao Paulo (USP)

Sao Paulo, Brazil

Abstract: After twelve years of stable operation, the Pierre Auger Observatoryhas collected a high quality and enhanced statistics data sample of ultra-highenergy cosmic rays, most of them with energies exceeding 1018 eV. Such datasample has improved our knowledge on several open issues in the field, such asthe spectral energy distribution of these ultra-relativistic particles, their chemi-cal identity, the levels of anisotropy imprinted in their arrival direction distribu-tion, and even the behaviour of hadronic interactions at centre-of-mass energies


above 50 TeV/nucleon, currently unreachable in particle accelerators. In thistalk, we start by presenting a general overview of the results of the Auger Obser-vatory related to the above mentioned topics. Next, the future upgrade plannedfor the Auger detectors, called AugerPrime, is discussed. It includes the instal-lation of plastic-scintillators at the top of each surface station, the operation ofan underground muon detector, a signal sampling with improved accuracy andlarger dynamic range using upgraded electronics, and also an extension of theduty cycle of the fluorescence detector. Altogether, these enhancements will pro-vide an improved determination of the electromagnetic and muon abundancesin air showers, which is currently a significant source of systematic uncertaintyin many of the data analyses. (email: [email protected])

Energy Spectrum of Cosmic Ray NucleiEak Raj Paudel

Tribhuvan University, Birendra Multiple CampusBharatpur Chitwan, Nepal

Abstract: The energy spectrum is heavily dominated by light nuclei . It hasbeen found that the lower energy cosmic ray flux is maximum than higher energycosmic ray flux for all types of nuclei under study. The relationship betweenmagnetic rigidity and flux value is also developed in this work. The magneticrigidity R of a particle is a measure of its resistance to a magnetic force thatdeflects the particle from straight line trajectory. (eak−[email protected])

Axisymmetric Magnetic Fields, Electron Capture andPycnonuclear Reactions in White Dwarfs

Edson Otoniel Da Silva*, Bruno Franzon, Manuel Malheiro, StefanSchramm, and Fridolin Weber

Instituto Tecnologico de Aeronautica (ITA)Sao Jose dos Campos, Brazil

Abstract: In this work, we study the properties of magnetized white dwarfs tak-ing into account possible instabilities due to electron capture and pycnonuclearfusion reactions in the cores of such objects. The structure of white dwarfs isobtained by solving the Einstein-Maxwell equations in a fully general relativis-tic approach. The stellar interior is composed of a regular crystal lattice madeof carbon ions immersed in a degenerate relativistic electron gas. The onsetsof electron capture reactions and pycnonuclear reactions are determined withand without magnetic fields. We find that magnetized white dwarf models vi-olate the standard Chandrasekhar mass limit significantly, even when electroncapture and pycnonuclear instabilities are present in the stellar interior. Weobtain a maximum white dwarf mass of around 2.12M , with a central mag-netic field of 1.74 × 1014G, which indicates that magnetized white dwarfs maybe the progenitor candidates of superluminous type Ia supernovae. (email*:[email protected])

A Vibration Isolation and Cooldown System for the Mirrors of theLaser Interferometric Gravitational Wave Detectors

Book of Abstracts 9

Elvis Camilo Ferreira*, Marcio Constancio Jr, Odylio Denys Aguiar,and Allan Douglas dos Santos Silva

Instituto Nacional de Pesquisas Espaciais (INPE)Sao Jose dos Campos, Brazil

Abstract: The direct detection of gravitational waves (GW) by the LIGO (LaserInterferometric Gravitational-Wave Observatory) inaugurated the GW astron-omy. The investigation of astrophysical objects and systems by GW requiresvery high sensitivity detectors, due to the relatively very small wave amplitudes.Therefore, it is necessary to reduce the effect of the detector noise sources.Therefore, we developed for the LIGO Voyager mirrors a vibration isolationand cooldown system using a Multi-Nested Pendula (MNP) with GeometricAnti-Springs. We present some results of the experimental tests of the MNPwith GAS, and thermal simulations to cool the interferometer mirrors down.(email*: [email protected])

QCD Dynamics of Proton-proton Scattering at Cosmic-rayEnergies

Emerson Gustavo de Souza LunaUniversidade Federal do Rio Grande do Sul (UFRGS)


Abstract: We present an eikonal model in which the energy dependence of theproton-proton total cross section is obtained from the QCD using a formulationcompatible with analyticity and unitarity constraints. More precisely, the be-havior of the total cross section is derived from the parton model using standardQCD cross sections for elementary parton-level processes, updated sets of quarkand gluon distribution functions and physically-motivated cutoffs which restrictthe elementary processes to semihard ones. We discuss the behavior of the scat-tering amplitude at very high energies within the QCD-based formalism andshow that the AUGER and Telescope Array results for the proton-proton totalcross section are well described by our eikonal model. (email: [email protected])

DUNE: next generation of precise measurements in neutrino sectorErnesto Kemp

Universidade Estadual de Campinas (UNICAMP)Campinas, Brazil

for the collaboration DUNE

Abstract: The last decade was remarkable for neutrino physics. In particular,the phenomenon of neutrino flavor oscillations has been firmly established bya series of independent measure-ments using solar, atmospheric, reactor andaccelerator neutrino beams. All parameters of the neutrino mixing matrix arenow known, and we have the elements to plan a judicious exploration of newscenarios that are opened by these recent advances. It is time to go further withprecise measurements to test the 3-neutrino paradigm and important questionslike the neutrino mass hierarchy and CP asymmetry in the lepton sector. Withinthis context the future long-baseline experiments are considered to be a funda-mental tool to deepen our knowledge of electroweak interactions. The Deep


Underground Neutrino Experiment - DUNE will detect a broad-band neutrinobeam from Fermilab in an underground massive Liquid Argon Time-ProjectionChamber at an L/E of about 103km/GeV to reach good sensitivity for CP-phase measurements and the determination of the mass hierarchy. The dimen-sions and the depth of the Far Detector also create an excellent opportunity tolook for rare signals like proton decay to study violation of baryonic number, aswell as supernova neutrino bursts, broadening the scope of the experiment toastrophysics and associated impacts in cosmology. In this presentation, we willdiscuss the physics motivations and the main experimental features of the DUNEproject required to reach its scientific goals. (email: [email protected])

Topics on Noncommutative CosmologyEverton Murilo Carvalho de Abreu

Universidade Federal Rural do Rio de Janeiro (UFRRJ)Rio de Janeiro, Brazil

Abstract: In this work we will analyze some issues concerning noncommuta-tive cosmology such as inflation, black holes and wormholes. We will see thatsome ideas like the age of the Universe and the radius of a black hole can bealtered. The wormholes discussed here have a rotational throat, and the angularmomentum is also altered thanks to the noncommutative feature of the space.However, it is important to stress that the physics of these objects and con-cepts suffer no modification in a noncommutative space-time background. Forexample, the accelerated characteristic of the Universe as well as the breakingof the energy rules by the wormholes are not modified, as well known. (email:[email protected])

From Helmholtz Theorem for Time-varying Vector Fields toGravito-electromagnetism Equations

Fabrıcio Tronco DalmolinUniversidade Tecnologica Federal do Parana (UFTPR)

Campus Medianeira, Brazil

Abstract: Among the results of the Einstein’s General Relativity there are theso famous Gravito-electromagnetism equations, so named because of the greatsimilarity with the Maxwell’s equations of electromagnetism. In general relativ-ity, these equations are derived from the pioneering work of Lense and Thirring[1] that through, a linearization of Einstein’s field equations for a rotating body,obtain the GEM equations. However, it is known from literature that the equa-tions have a serious problem of divergence [2,3,4,8], which leads to violationthe unicity of the fields. In this work we start from the Helmholtz theoremfor time-varying vector fields [5,6] in order to obtain the GEM equations by amore general way, supported on a mathematical theorem. Finally we discussthe results and the main differences between them and those obtained fromthe general relativity. References: [1] J. Lense and H. Thirring : Phys. Z. 19(1918) 156.[ English translation by B Mashhoon et al., Gen. Rel. Grav. 16(1984) 711]. [2] A. Tartaglia e M. L. Rugiero, Gravito-eletromagnetism versusEletromagnetism, Eur. J. Phys. 25 (2004) 203-210. [3] Hans C. Ohanian, R.Ruffini, Gravitation and Spacetime, W. W. Norton and Company, New York,

Book of Abstracts 11

(1994). [4] Misner C. W., Thorne K. S., Wheeler J. A., Gravitation, FreemanEd., S. Francisco, (1973). [5] Davis M., A Generalized Helmholtz Theorem forTime-varying Vector Fields, AJP, 74, 72 (2006). [6] J. A. Heras, Comment on“A generalized Helmholtz theorem for time-varying vector fields,” by Artice M.Davis, Am. J. Phys.74, 72-76 (2006). [7] J. D. Oleg, Gravitation and Cograv-itation, Electret Scientific Company Star City, (see in particular charpter 3),(2006). [8] Donato Bini, Christian Cherubini, Carmen Chicone and BahramMashhoon, Gravitational Induction, Classical and Quantum Gravity, Volume25, Number 22. (email: [email protected])

Rotation-driven Phase Transitions in the Cores of Neutron StarsFridolin Weber*, W. Spinella, and O. Zubairi

San Diego State University (SDU)San Diego, USA

Abstract: In this talk, I will discuss the impact of rapid rotation of neutronstars on the structure of the matter deep inside their central cores. The studyis based on recent models for the nuclear equation of state, whose parametersare tightly constrained by nuclear data, neutron star masses, and the latestestimates of neutron star radii. (email: [email protected])

Orbits Around Asteroids Found Through Poincare Surface ofSection

Gabriel Borderes MottaFaculdade de Engenharia de Guaratingueta, Universidade Estadual Paulista

(FEG/UNESP)Guaratingueta, Brazil

Abstract: Missions that intend study small bodies like asteroids and cometshas increased in number over the past few years. To model the gravitationalpotential of irregular bodies there is the spherical harmonics model, but thismodel is useful just at large distances. Another way to model the gravitationalpotential is by the constant density polyhedron model. In this work we adoptanother gravitational potential model that is called mass concentration (mas-cons) model and consist in set points with mass as way to reproduce a asteroidshape. Integration of a particle orbit can be compute with this model. The wayto look for interesting orbits for different missions in this work is the Poincarsurface of section. An asteroid was chosen and different orbits around it wereanalyzed. (email: gabriel−[email protected])

Stability of Charged White DwarfsGeanderson Araujo Carvalho*, Jose Domingo Arbanil Vela,

Rubens M. Marinho Jr, and Manuel MalheiroInstituto Tecnologico de Aeronautica (ITA)


Abstract: Recently were discovered superluminous type Ia Supernovae [1][2] inwhich some authors suggest that their progenitors have a mass that exceed the


Chandrasekhar mass limit. In view of this we follow the idea that a net chargedistribution can generate theoretically white dwarfs with a mass that signifi-cantly exceed the Chandrasekhar mass limit [3]. In this work we did a betterestimative of the effect of a net charge distribution in a general relativistic con-text being more carefully about the effects of the net charge to the Equation ofState (EoS) for White Dwarfs and how this net charge distribution is relatedto mass distribution in such stars. Finally we use Tolman-Oppenheimer-Volkoffequation to find a mass-radius relation for these stars and we use radial oscilla-tions equations to study their stability using general relativity. The conclusionsabout this work are still object of discussion. [1] D. A. Howell et al., Nature(London) 443, 308 (2006). [2] R. A. Scalzo et al., Astrophys. J. 713, 1073(2010). [3] H. Liu et al., Phys. Rev. D 89, 104043 (2014). (email*: [email protected])

Quark-hadron Phase Transition in Proto-neutron Stars CoresBased on a Non-local NJL Model

German Malfatti*, G. Contrera, M. Orsaria, and Fridolin WeberFacultad de Ciencias Astronomicas y Geofısicas

Universidad Nacional de La Plata (INLP)Buenos Aires, Argentina

Abstract: We study the QCD phase diagram using a non-local SU(3) NJL modelwith vector interactions among quarks. We analyze the thermodynamic quan-tities such as entropy and specific heat and the influence of vector interactionsin the phase transition process. Theoretical studies show that vector interac-tions stiffen the equation of state of cold hybrid stars. By considering electriccharge neutrality and baryon number conservation, we build the equation ofstate for the core regions of proto-neutron stars and discuss the astrophysicalimplications of considering this non-local quark model. (email*: [email protected])

Magnetized Neutron StarsGibran Henrique de Souza*, Ernesto Kemp, and Cecilia Chirenti


Abstract: Here we solve numerically the relativistic Grad-Shafranov equation,that describes the vector potential behavior, for a typical neutron star having asequation of state the matter described by Akmal, Pandharipande and Ravenhall(APR2). (email*: [email protected])

Investigating the Prompt Photon Production at the LHC EnergiesGlauber Sampaio dos Santos* and M. V. T. Machado


Abstract: We investigate the rapidity and transverse momentum distributions ofthe prompt photon production at the LHC energies considering the color dipole


approach. We compare the predictions from distinct models for the dipole crosssection, where parton saturation models at high energies are expected to beimportant at the forward rapidities in pp and pA collisions at the LHC. (email*:[email protected])

TitleGuilherme Goncalves Ferrari


Abstract: (email*: [email protected])

Mimetic Dark Matter in Pseudo-complex General RelativityGuilherme Lorenzatto Volkmer* and Dimiter Hadjimichef


Abstract: We investigate the dark matter problem in the context of Pseudo-complex General Relativity. A form of gravitational dark matter has recentlybeen studied, the mimetic dark matter, which is a scalar tensor extension forgravity where the conformal degree of freedom is isolated in a covariant way. Forsuch, we perform a combination of both approaches to reveal non trivial resultseven in the absence of matter. Solutions for different scenarios and possibleinterpretations are presented. (email*: volkmer−@hotmail.com)

Hybrid Stars in the Framework of NJL ModelsGustavo A. Contrera*, Milva G. Orsaria, Ignacio F.

Ranea-Sandoval, and Fridolin WeberInstituto de Fısica de La Plata

Universidad Nacional de La Plata (UNLP)La Plata, Argentina

Abstract: The discovery of the two-solar mass neutron stars J1614-2230 (1.97±0.04M⊙) and J0348+0432 (2.01± 0.04M⊙) allows the possible existence of de-confined quarks in the cores of neutron stars. We compute the equation ofstate of the matter in the cores of hybrid stars for hadronic matter, treated inthe non linear relativistic mean-field approximation and quark matter, repre-sented by three-flavor local and non-local Nambu-Jona-Lasinio (NJL) modelswith repulsive vector interactions. The transition of hadronic to quark mat-ter (mixed phase) is constructed by considering either a soft phase transition(Gibbs construction) or a sharp phase transition (Maxwell construction). Wefind that high-mass neutron stars with masses up to 2.1 − 2.4M⊙ may con-tain a mixed phase in their cores, if global charge conservation is consideredthrough the Gibbs conditions. However, if the Maxwell condition is considered,the appearance of a pure quark matter core e ither destabilizes the star imme-diately (typically for non-local NJL models) or leads to a very short hybrid starbranch in the mass-radius relation (usually for local NJL models). Our study


also indicates that neutron stars with masses of around 1.4M⊙ would not con-tain deconfined quark matter. Very good agreement with the thermal evolutionestablished for the neutron star in Cassiopeia A (Cas A) is obtained for one ofour models, if the protons in the core are strongly paired, the repulsion amongthe quarks is mildly repulsive, and the mass of Cas A has a canonical value of1.4M⊙. (email*: [email protected])

A model of the Breaking Index of PulsarsHeitor Oliveira de Oliveira*, Rubens de Melo Marinho Jr,

and Nadja Simao MagalhaesInstituto Tecnologico de Aeronautica (ITA)


Abstract: In this work we present our proposal of a model for pulsars’ rotationfrequency decay by modifying an assumption of the canonical model. Startingfrom the model of spin powered pulsars, where the electromagnetic energy isprovided by the rotational energy, we explore the influence of the variationof the star radius on the value of the braking index considering a theoreticalmodel. We find that the braking index gets smaller as the star radius increases,also implying a higher moment of inertia. This contribution does not alter theemission of magnetic dipole energy but reduces the star’s angular velocity andconsequently, the frequency of the light pulses of the pulsar, as is observed.We tested our model with data of seven pulsars with observed braking indices,obtaining good results. (email*: [email protected])

Atmospheric Tidal Effects on Cosmic Ray Shower ProductionHelio Takai

Brookhaven National LaboratoryUpton, Nova Iorque, USA

Abstract: Elementary particle production by cosmic rays in the Earth’s atmo-sphere is a well understood process. High energy cosmic rays collide with theelemental constituents of the atmosphere producing a shower of particles. Themultiplicity, species distribution, and their energy spectra are a function of theincident cosmic ray energy and type. The point of production and flux measuredat various altitudes depends on the atmospheric density profile as function ofaltitude. Using data of muon flux collected for the past eight years, and at-mospheric data from various sources, we study the close relationship betweenthe atmospheric conditions and particle production. Atmospheric tidal effectsare clearly observed in our data as seasonal and daily modulation of the muonflux. We will present the results of the analysis and discuss the importanteof including a detailed description of the atmosphere in interpreting data fromexperiments searching for non standard model particles. (email: [email protected])

Magnetic suspension with motorization to measure the speed ofgravity.

Henrique Linares*, Carlos Frajuca, Givanildo Alves dos Santos,and Franscisco Yastami Nakamoto


Instituto Federal de Educacao, Ciencia e Tecnologia de Sao Paulo (IFSP)Sao Paulo, Brazil

Abstract: This work aims to design a magnetic suspension for an experiment tomeasure gravity’s velocity. Such device must rotate two objects symmetricallywith the greatest mass and largest radius as possible, at the speed of 500,000rpm, which means this device falls into the high-speed machines category. Theguidelines and solutions proposed in this paper constitute a contribution to thisclass of engineering problems and were based on an extensive literature search,contacts with experts, the tutor’s and author’s experience, as well as on experi-mental results. The main solution proposed is a hybrid bearing that combines aradial passive magnetic bearing with an axial sliding bearing, here called MPS(Magnetic Passive and Sliding) bearing. (email*: [email protected])

Piercing the Vainshtein Screen with Anomalous GravitationalWave Speed: constraints on modified gravity from binary pulsars

Hermano Velten*, J. Beltran, and F. PiazzaUniversidade Federal do Espırito Santo (UFES)

Vitoria, Brazil

Abstract: By using observations of the Hulse-Taylor pulsar we constrain thegravitational wave (GW) speed to the level of 10−2. We apply this result toscalar-tensor theories that generalize Galileon 4 and 5 models, which displayanomalous propagation speed and coupling to matter for GWs. We argue thatthis effect survives conventional screening due to the persistence of a scalar fieldgradient inside virilized over-densities, which effectively “pierces” the Vainshteinscreening. In specific branches of solutions, our result allows to directly constrainthe cosmological couplings in the effective field theory of dark energy formalism.[PRL 116, 061101 (2016)] (email*: [email protected])

TitleIvana de Freitas Cunha

Instituto Tecnologico de Aeronautica (ITA), Sao Jose dos Campos, Brazil

Abstract: (email: cunha−[email protected])

Recent Advances in Conformal GravityJames G. O’Brien

Wentworth Institute of Technology (WIT)Boston, USA

Abstract: In recent years, significant advances have been made in alternativegravitational theories. Although MOND remains the leading candidate amongstthe alternative models, Conformal Gravity has been studied by Mannheim andO’Brien to solve the rotation curve problem without the need for dark matter.Recently, Mannheim, O’Brien and Chaykov have begun solving other gravi-tational questions in conformal gravity. In this presentation, we first reviewConformal Gravity. Second, we highlight the new work of Conformal Grav-ity’s application to random motions of clusters (the original Zwicky problem),


gravitational bending of light, gravitational lensing and a very recent surveyof dwarf galaxy rotation curves (bringing the total count of rotation curves fitby conformal gravity to over 200). We will show in each case that conformalgravity can provide an accurate explanation and prediction of the data withoutthe need for dark matter. Coupled with the fact that Conformal Gravity is afully renormalizable metric theory of gravity, these results help to push confor-mal gravity onto a competitive stage against other alternative models. (email:[email protected])

Combustion of Hadrons to Strange Quark Matter Inside a NeutronStar

Jhon Andersson Rosero Gil*, J. A. Rosero, E. Kemp, and GLugones

Universidade Federal do ABC (UFABC)Santo Andre, Brazil

Abstract: We have studied the phase transition from hadronic to quark matterinside neutron stars. The transition starts with the deconfinement of quarksdriven by strong interactions, and is followed by the weak interaction decay ofquarks until the chemical equilibrium. We have calculated the rate of all therelevant weak interaction processes and solved the Boltzmann equation, consid-ering the effect of strong interactions in the perturbative regime to the order ofQCD coupling constant and also the effect of finite temperature and strangequark mass. The result shows that the transition has a significant influence onthe increasing of the core temperature, the particle abundances and the ener-gies of neutrinos emitted by unstable beta particles, which is of the order of theenergy released during the supernova explosion. (email*: [email protected])

Observing Relativistic Effects Near Compact Objects with MIRAXJoao Braga

Instituto Nacional de Pesquisas Espaciais (INPE)Sao Jose dos Campos, Brazil

Abstract: The observation of X rays coming from the inner regions of the accre-tion flow onto compact objects like neutron stars and black holes is a powerfultool to probe general relativistic effects. Precise timing of the X-ray flux canunveil frequencies associated with motion under Kerr metric like Lense-Thirringprecession, Bardeen-Peterson effect and periastron precession. Spectral fittingcan provide important information about the spin of black holes thought thedetermination of the radius of the innermost stable circular orbit (ISCO) of theaccretion disk. Distorted emission lines can also probe the transverse Dopplershift and the gravitational redshift. In this work we shot the contribution thatthe MIRAX mission will be able to make toward measuring these effects onGalactic X-ray binaries and supermassive black holes in Active Galactic Nuclei.([email protected])

A Small STEP that May Rock our MOND(e) and Render MattersLess Dark


Jonas Pedro PereiraUniversidade Federal do ABC

Santo Andre, Brazil

Abstract: It has been recently pointed out [PRL 117, 071103 (2016)] that,besides the universality of free fall, the Earth-based experiment called SatelliteTest of the Equivalence Principle (STEP) can also test Newton’s second lawof motion (MOdified Newtonian Dynamics, MOND) with its currently planneddesign and sensitivity. We discuss the importance, nontriviality and implicationsof that mainly in the contexts of fundamental physics and dark matter. (email:jonaspedro−[email protected])

Inside Real Neutron Stars: observations and theory of pulsarcrusts/magnetospheresJorge Ernesto Horvath

Abstract: We review in this talk the issue of pulsar timing irregularities, gen-erally tied to the existence of superfluid components in the (solid) crust of thestar. We show how these data is useful to characterize and constrain this crust,and also how non-standard torques may be required to fully explain the trajec-tories of pulsars in the P −P plane, with possible consequences for the existenceof magnetars. (email: [email protected])

Three-body Heavy Meson Decays with Final State Interactionsand CP Violation

Jorge Henrique de Alvarenga Nogueira* and Tobias FredericoInstituto Tecnologico de Aeronautica (ITA)


Abstract: The formation of CP violation (CPV) constrained by CPT invarianceis affected by resonances and final state interactions (FSI). Starting from theCPT constraint, a generalized CP asymmetry formula including resonances andFSI is computed without the three-body FSI contribution. A simple B decaymodel is elaborated with the ρ and f0(980) resonances plus a non resonantbackground including the ππ → KK coupled amplitude. Performing the fit ofthe CP asymmetry for one charmless three-body B± decay channel the formulapresents fair agreement with the high statistics LHCb data in the mass regionbelow 1.6 GeV and we obtain as outcome a coupled decay channel for thechannel asymmetry. The model is extended to study the CP violation in thehigh mass energy region. The CPV occurring in this sector of the phase spacecould be associated with the final state interaction coupling the pair of lightpseudo-scalars to double charm B decay channels. We also discuss the threebody final state interaction (FSI) contribution to B decay within a light-frontframework, considering S-wave interactions decomposed in isospin states. Theconvergence of the re-scattering series can be checked computing terms in anincreasing perturbative order. (email*: [email protected])

Minkowski space structure of a bosonic bound state with anon-planar interaction kernel


Jorge Henrique Alvarenga Nogueira*, V. Gigante, E. Ydrefors, C.Gutierrez, V.A. Karmanov, T. FredericoInstituto Tecnologico de Aeronautica (DCTA)

Sao Jose dos Campos, BrazilInstituto de Fısica Teorica (UNESP)

Sao Paulo, BrazilLebedev Physical Institute, Leninsky Prospekt 53, 119991 Moskow, Russia

Abstract: The nonperturbative aspects of a relativistic bound system can beinvestigated by its structure in the Minkowski space. Applications to QCD areusually done in Euclidean space by means of the Wick rotation, which allowsto simplify the bound state problem, but limits the computation of observablesdefined in Minkowski space. We study the relativistic system of two scalar parti-cles using the Bethe-Salpeter amplitude in Minkowski space, in order to preparefuture applications to explore the nonperturbative physics of QCD. Within thehomogeneous Bethe-Salpeter equation, using the Nakanishi representation forthe associated amplitude and projecting onto the light-front, which leads to anon-singular integral equation, the problem is solved numerically. The interac-tion kernel is considered with the ladder (L) plus non-planar cross-ladder (CL)contributions. We compare and discuss our calculations with the nonperturba-tive study of generalized ladder graph made in Ref. [tjon]. We also compute theelectromagnetic form factor, including, besides the impulse approximation, thetwo-body current contribution, associated with higher Light-Front Fock states.In addition, the valence Light-Front wave function is calculated, which allowsto compute the parton momentum distributions. These observables are intrin-sically connected with the Minkowski space structure. We note that althoughsome features of these quantities, which are related with the binding energycan be computed in Euclidean space, allowing some understanding of the effectcoming from the infinity set of crossed-ladder diagrams that contributes to theinteraction kernel. To illustrate some of these effects in QCD, we add the colordegree of freedom to the bosonic system to study the suppression of the non-planar diagrams in the large Nc limit [thooft]. The suppression is importantto a planar description when applying the model to strong interactions, and wesearch for specific effects in the structure. (email*: [email protected])

References: [tjon] T. Nieuwenhuis and J. A. Tjon, Nonperturbative Study ofGeneralized Ladder Graphs in a ϕ2χ Theory, Phys. Rev. Lett. 77, 814 (1996);[thooft] G. t’ Hooft, A Planar Diagram Theory for Strong Interactions, Nucl.Phys. B 72, 461-473 (1974)

Dormant Black HolesJose Antonio de Freitas Pacheco

Observatoire de la Cte d’Azur (OCA), Brazil

Abstract: Supermassive black holes in the center of galaxies can be in a dormantstate, that is not accreting matter. These black holes manifest from time to timean electromagnetic or gravitational activity by tidally disrupting nearby stars orby capturing compact objects like neutron stars or stellar black holes. I discussthese processes providing the expected rate of gravitational wave signals andthe light curve for tidal events. (email: [email protected])


Delta Resonance Coupling with Waleckas Mesons: implications tostellar matter EoS

Jose Carlos Teixeira de Oliveira*, William Silva Gomes, HilarioRodrigues, and Sergio Barbosa DuarteUniversidade Federal de Roraima (UFRR)

Boa Vista, Brazil

Abstract: In this work we have obtained the equation of state to the highlyasymmetric dense stellar matter, using the nonlinear Walecka model in themean field approximation. We discussed the implication of changes in couplingconstant of the delta baryonic resonance on the observable of the neutron star.A detailed analysis of the equation of state and of the baryonic effective massin respect to changes in the delta coupling constants is carried out. We focusattention on a new aspect observed for pressure when varying the baryonicdensity of the medium; a first order phase transition like a liquid-gas phasetransition was observed for an acceptable range of delta coupled constant values.We have explored the implication of this aspect for the neutron star structureand their maximum masses. (email*: [email protected])

Recent Babar Results on Time-reversal and CP AsymmetriesJustin Albert

University of VictoriaVictoria, Canada

Abstract: We present a selection of recent results on time and CP asymmetriesmeasured with the BaBar detector. They include measurement of T and CPasymmetries in the B0 − B0 mixing process using inclusive dilepton samples, atest of CPT symmetry using B0 decays to ccK0, and a Dalitz plot analysis of thecharmless decay B+ → Ksπ

+π0, where the first evidence of direct CP violationin the B+ → K∗+π0 decay has been seen. We also present a measurement ofthe parameter sin(2β) of the Unitarity Triangle in B0 → D0h0 decays, whichmakes use of the combined data sets of the BaBar and Belle experiments. (email:[email protected])

ALTAIR: precision photometric calibration via artificial lightsources above the atmosphere

Justin AlbertUniversity of Victoria

Victoria, Canada

Abstract: Understanding the properties of dark energy via SNIa surveys, andto a large extent via other methods as well, requires unprecedented photometricprecision. Laboratory and solar photometry and radiometry regularly achieveprecisions on the order of parts in ten thousand, but photometric calibration fornon-solar astronomy presently remains stuck at the percent or greater level. AL-TAIR (http://projectaltair.org) is beginning to erase this discrepancy, providingsteps toward achieving laboratory-level photometric precision for major sky sur-veys at the end of this decade. In particular, we show far- and near-field imaging


of the balloon-borne light source we presently launch to altitudes of approxi-mately 20 km, and our initial calibration results, in addition to our prior workwith a present calibrated source in low-Earth orbit. The ALTAIR techniqueis additionally applicable to microwave astronomy: observation of gravitationalwaves in the polarized CMB will similarly require unprecedented polarimetricand radiometric precision, and we briefly present our plans for a calibratedmicrowave source above the atmosphere as well. (email: [email protected])

Gamma Ray Bursts and Stellar EvolutionKauan Dalfovo Marquez* and Debora Peres Menezes


Abstract: Gamma ray bursts are distinguished mainly by their duration and theenergies released and they are known as soft (SGRBs) and long (LGRBs) gammaray bursts. The total nergy released in the first few hundred seconds is of theorder of 1050 erg, which is two or three orders of magnitude smaller than seenin LGRBs. Not long ago it was proposed that LGRBs can be a manifestationof a phase change in the interior of a neutron star, causing a conversion of ahadronic star into a quark star. Recent observational results, as the existenceof 2 M⊙ neutron stars with relatively small radii, have constrained relativisticequations of state (EOS) from more than two hundred to about 3 dozens. Theenergetics of the LGBRs will be revisited and only accepted EOS will be used.The results will be confronted with the results of the released energy in LGRBs.(email*: [email protected])

Statical Properties of CMB B-mode PolarisationLarissa Carlos de Oliveira Santos*, Y. R. Hu, K. Wang and W. Zhao

University of Science and Technology of China (USTC)Hefei, China

Abstract: The next target of cosmic microwave background (CMB) experimentsis the detection of the primordial B-mode polarisation signal generated by gravi-tational waves (GWs) in the early universe, as predicted by inflationary models.However, GWs are not the only source of B-mode polarisation in CMB: weakgravitational lensing of the CMB photons due to large-scale structure along theline of sight converts part of E-mode polarisation into B-mode component. Inaddition, foreground residuals can mimic CMB B-mode polarisation and mustbe studied in detail. Moreover, in a realistic point of view, the CMB B-map mustbe generated from partial sky maps due to Galactic contaminations even in thecase of satellite surveys. The incomplete sky coverage leads to the so called E-to-B leakage that increases the uncertainty of the estimated primordial B-modesignal. Therefore, considering the LCDM model, the total B-mode map is thena non-Gaussian field due to different contaminations to the gaussian primordialsignal. For non-gaussian fields, in addition to the power spectrum, other statis-tics must considered, as for example the Minkowski Functionals (MFs). We willuse the MF as a tool to study the imprint of different components in the totalB-mode map, especially the E-to-B leakage. (email: [email protected])


Nucleosynthesis in Strange Star MergersLaura Paulucci*, J.E. Horvath, and O. Benvenuto

Universidade Federal do ABC (UFABC)Santo Andre, Brazil

Abstract: The possible existence of deconfined matter in the cores of neutronstars has been studied for over three decades without a firm indication eitherfor or against this proposition. Analysis mostly rely on the comparison of mass-radius curves obtained for different compositions with observational data on themass of the most massive objects of this kind accurately determined. Neverthe-less, there are other possibilities for indirectly studying the internal compositionof this class of compact objects, e.g, analyzing cooling behavior, X-ray bursts,supernova’s neutrinos. We present calculations on the expected nucleosynthesisspectra for the strange star-strange star merger scenario as means to test thestrange quark matter hypothesis and its realization inside such objects. Thiswould result very different from the typical r-process nucleosynthesis expected inneutron star mergers since the high temperature deconfinement of strange mat-ter would produce large amounts of neutrons and protons and the mass buildupwould proceed in a Big-Bang nucleosynthesis like scenario with a higher neutronto proton ratio. Results are then evaluated for its viability as an explanationfor the observables, mainly the elemental abundances and light curve. (email*:[email protected])

Strange star - strange planet binary systems as sources ofgravitational and electromagnetic waves

Lilian de Araujo Ferrao*, Pedro H.R.S. Moraes,and Manuel M.B.M. Oliveira

Instituto Tecnologico da Aeronautica (ITA)Sao Jose dos Campos, Brazil

Abstract: Recently gravitational waves were directly detected for the first time[Abbott, B.P. et al., Phys. Rev. Lett. 116 061102 (2016)]. The progenitorsystem of such waves was a binary black hole. Those systems as well as binaryneutron star systems are among the most promising gravitational waves sourcefor detectors like Advanced LIGO and VIRGO. Also recently it was shownthat a binary system made of a strange star and a strange planet could be animportant source of gravitational waves to be observed by Advanced LIGO,VIRGO and futures detectors [Geng, J.J., Astrophys. J. 804 21 (2015)]. Ourwork consists in verify whether this type of system is numerous enough in theuniverse to be considered an important source of gravitational waves. Besides,we intend to verify the observational counterpart that can be expected for thiskind of event. Thereby, the existence of such systems could be confirmed withthe gravitational wave detection of their coalescence followed by the observationthrough telescopes in X and gamma-rays and even visible light telescopes. Withthis counterpart, besides confirming the existence of strange star, strange planetbinary systems, the existence of strange matter can be proved as the groundstate of matter at high energies. (email: [email protected])

Cosmic-magnetism in Alternative Theories of Gravity


Luiz Garcia de AndradeUniversidade do Estado do Rio de Janeiro (UERJ)

Rio de Janeiro, Brazil

Abstract: The present status of cosmic magnetism is briefly reviwed andnew results presented based on the works of K Bamba and myself with specialenphases of cosmoc magnetic seeds and dynamos in torsion cosmology. (email:[email protected])

Detonation wave by hadron-quark phase transitioninto compact stars

Luis Gustavo de Almeida*, Hilario A. Rodrigues,and Sergio B. Duarte

Universidade Federal do Acre (UFAC)Rio Branco, Brazil

Abstract: In this work we present an effective description of the detonation waveformation in hadronic matter inside a proto-neutron star core. We have used asimplified two shell model where the inner shell medium is initially composedof a small lump of strange quark matter surrounded by a thick outer shellcomposed of hadronic matter. We have used an equation of state (EOS) basedon Relativistic Mean Field Theory with the coupling parameter set NL3 todescribe the nuclear phase and a Virial expansion to describe the subnuclearphase. We used the MIT bag model to describe the strange quark matter. Thehadron-quark phase transition actually induces highly non equilibrium modes,which may become a detonation process (faster) or a burning process (slower).The main purpose of the work is to study the formation of a remnant quarkstar and the possibility of mass ejection caused by the hadron-quark phasetransition. We have found that the total amount of ejected mass is dependenton the bag model constant used in the strange matter description. (email*:[email protected])

Luminosity Function Statistics Applied in GRB SamplesLuis Juracy Rangel Lemos*, Remo Ruffini, and Carlo Bianco

Universidade Federal do Tocantins (UFT)Palmas, Brazil

Abstract: The luminosity function (LF) statistics applied in data of GRBs de-tected by GBM/Fermi and BAT/Swift is the theme approached in this work.The LF is a strong statistical tool to extract useful information from astro-physical samples, and the key point of this statistical analysis is in the detectorsensitivity, where we have performed careful analysis. We produced, by LFstatistics, the GRB predicted distributions of: peak ux N(Fpk), redshift N(z)and peak luminosity N(Lpk). We also used differents GRB rates. We performeda comparison between the distributions predicted and observed (with and with-out redshifts), where we had to build a list with more then 250 GRBs withknown redshifts. We estimated the effects of the Malmquist bias in all samples,and we looked for a correlation between the isotropic luminosity and the Bandpeak spectral energy. (email*: [email protected])


Total, Elastic and Single Diffractive Cross Sections for LHCEnergies in Miettinen-Pumplin Model

Mairon Melo Machado* and Magno Valerio Trindade MachadoInstituto Federal de Educacao Ciencia e Tecnologia do Rio Grande do Sul (IF

Farroupilha)Farroupilha, Brazil

Abstract: In this contribution we provide predictions for total, elastic and singlediffractive cross sections calculated to proton-proton collision at LHC energies(in centre-of-mass energy 0,9 TeV, 7 TeV, 8 TeV and 14 TeV) considering theframework from the Miettinen-Pumplin model. Such an approach has correctlydescribed the data available at Fermilab-Tevatron energies. Our predictions arebased on E811 and CDF σtot and σel data, which gives about 10% of the totalcross sections for the diffractive cross sections in all range of energies, and it is inagreement with the CERN-ATLAS Collaboration experimental result. (email*:[email protected])

Magnetars and White Dwarfs PulsarsManuel Malheiro

Departamento de Fısica, Instituto Tecnologico de Aeronautica (ITA)Sao Jose dos Campos, Brazil

Abstract: Some of the most interesting types of astrophysical objects thathave been intensively studied in the recent years are the Anomalous X-ray Pul-sars (AXPs) and Soft Gamma-ray Repeaters (SGRs) seen usually as neutronstars pulsars with super strong magnetic fields, known as magnetars. However,in the last years three SGRs with low magnetic fields have been detected. More-over, three fast and very magnetic white dwarfs have also been observed in thelast years. Based on these new discoveries, massive highly magnetized rotatingwhite dwarfs (WDs) have been proposed as an alternative explanation to the ob-servational features of SGRs and AXPs [1,2], in total analogy with pulsars pow-ered by rotating neutron stars (NSs).The properties of magnetic white dwarfs arecomputed for an equation of state which describes white dwarf matter in terms ofa regular crystal lattice of atomic nuclei at zero temperature, immersed in a to-tally magnetized electron gas. The minimum critical densities at which electroncapture reactions and possibly pycnonuclear fusion reactions occur inside of ro-tating white dwarfs are studied for different magnetic fields and stellar rotationrates. Furthermore, an analysis of the possibility of radio emission was done forthe 23 Magnetars in order to find an explanation for the puzzle why for almostall the SGRs/AXPs were expected radio emission, but it was observed only infour of them [3]. Finally, we also investigate the energy source for these starsconsidering them as rotation powered pulsars, computing their structure prop-erties, from numerical integration of the self-consistent axisymmetric generalrelativistic equilibrium equations by making use of selected up-to-date nuclearequations of state. [1] - M. Malheiro, J.A. Rueda, and R. Ruffini, Publicationsof the Astronomical Society of Japan, Vol.64, No.3, Article No.56, 13 pp (2012)http:// adsabs.harvard.edu/abs/2012PASJ...64...56M; [2] - J.G. Coelho and M.Malheiro Publications of the Astronomical Society of Japan, Volume 66, Issue1, id.14 (2014) http://adsabs.harvard.edu/ abs/2014PASJ...66...14C [3] - RV


Lobato, JG Coelho, M Malheiro, Radio pulsar death lines to SGRs/AXPs andwhite dwarfs pulsars - THE SECOND ICRANET CESAR LATTES MEETING,AIP Conf. Proc. 1693, 030003 (2015). (email: [email protected])

The Effect of the Anisotropy on the Stability of Strange StarsManuel Malheiro and Jose Domingo Arbanil Vela*

Instituto Tecnologico da Aeronautica (ITA)Sao Jose dos Campos, Brazil

Abstract: The influence of the anisotropy in the equilibrium and stability ofstrange stars is investigated through the numerical solution of the hydrostaticequilibrium equation and the radial oscillation equation, both modified fromtheir original version to include these effects. Two different kinds of localanisotropic equations of state are considered. One that is non-null at the star’ssurface and other one that is null on it, namely, σs = 0 and σs = 0. Whenσs = 0, we found that in strange stars the central energy density used to reachthe maximum mass value is the same used to determine the zero frequency ofoscillation, indicating of this way that the maximum mass marks the onset ofthe instability. In turn, when σs = 0, the maximum mass point and the zerofrequency of oscillation are derived from the same central energy density onlyin a sequence of stars with the same value σs. I.e., in a sequence of equilib-rium configurations with the same value of σs, the regions constituted by stableand unstable configurations against radial oscillations can be determined al-ways by the conditions dM/dρc > 0 and dM/dρc < 0, respectively. (email*:[email protected])

Ansatz for Dense Matter Equation of StateMarcelo Dallagnol Alloy, Manuel Malheiro,

and Debora Perez MenezesUniversidade Federal de Santa Catarina (UFSC)

Florianopolis, Brazil

Abstract: Recently, two massive pulsars were observed, PSR J1614-2230 andPSR J0348+0432, causing excitement between theorists. The first one wasobserved in 2010 with mass (1.97 ± 0.04) solar masses and the second onewas observed in 2013 with mass (2.01 ± 0.04) solar masses. The maximummass of a neutron star is a very important constraint in the description ofdense matter. In this work, we assume that the equation of state is given byp = Aec + Be, where p is the pressure, e is the energy density, and A, B andC are free parameters that we vary in order to satisfy both the TOV equationsand the baryonic density restricted to theoretical and observational constraints.(email: [email protected])

Gravitational Waves in Running Vacuum CosmologiesMarcio Eduardo da Silva Alves*, D.A. Tamayo, J.A.S. Lima,

and J.C.N. de AraujoInstituto de Ciencia e Tecnologia, Universidade Estadual Paulista

(ICT/UNESP)Sao Paulo, Brazil


Abstract: We investigate the cosmological production of gravitational wavesfor a nonsingular flat cosmology driven by a decaying vacuum energy density.The model studied can be interpreted as a particular case of the class recentlydiscussed by Perico et al. (Phys. Rev. D 88, 063531, 2013) which is termedcomplete in the sense that the cosmic evolution occurs between two extremede Sitter stages (early and late time de Sitter phases). The gravitational waveequation is derived and its time-dependent part numerically integrated sincethe primordial de Sitter stage. The transition from the early de Sitter to theradiation phase is smooth (no exit problem) and the generated spectrum ofgravitons is compared with the standard calculations where an abrupt transitionis assumed. It is found that the stochastic background of gravitons is very similarto the one predicted by the cosmic concordance model plus inflation except forthe higher frequencies (f 100 kHz). This remarkable signature of a decayingvacuum cosmology combined with the proposed high frequency gravitationalwave detectors of improved sensitivity may provide in the future a crucial testfor inflationary mechanisms. (email*: [email protected])

Time Variability of NS-LMXBs as Oscillation Modes ofRelativistic Axisymmetric Tori: implications for constraining the

parameters of neutron starsMarcio Guilherme Bronzato De Avellar*, L. Rezzolla, O. Porth,

and Z. YounsiInstitute for Theoretical Physics - Goethe University

Frankfurt am Main, Germany

Abstract: There have been many efforts to explain the dynamical mechanismsand models for the origin and phenomenology of the quasi-periodic oscillations(QPOs) seen in the X-ray light curves of low-mass X-ray binaries. Up to now,none of the models on the market can address all the frequencies observed inthe power density spectrum of the light curve. However, new light is shed onthe problem through sophisticated simulations of accretion flows onto compactobjects. We perform several hydrodynamic simulations of non-self gravitatingrelativistic axisymmetric thick tori around the neutron star in the low-mass X-ray binary 4U 1636-53 and show how the observed oscillation modes triggeredby different velocity perturbations give rise to a set of variability features simi-lar to what we see in the observational X-ray data, in particular in the case ofthe kiloHertz QPOs. We compare the simulated and the observational relationsbetween the upper and lower kiloHertz QPOs frequencies to probe the inner re-gions of the system, potentially constraining the mass and radius of the neutronstar. (email*: [email protected])

Braneworld Scenarios from Deformed Defect ChainsMariana Chinaglia*, Alex de Bernardini, and Roldao da Rocha

Universidade Federal de Sao Carlos (UFSC)Sao Carlos, Brazil

Abstract: Novel braneworld scenarios supported by warp factors driven by asingle extra dimension are obtained from deformed one-dimensional lump-likesolutions known a priori. Through a novel ansatz, the internal energy structure,


the braneworld warp factor, and the quantum mechanical analogue problem,as well as the associated zero mode solutions, are straightforwardly derivedby means of an analytical procedure. The results allow one to identify thickbrane solutions that support internal structures and that can hold the (3 +1)-dimensional gravity. (email*: [email protected])

Regge Phenomenology at LHC EnergiesMateus Broilo*, C.A.S. Bahia, and E.G.S. LunaUniversidade Federal do Rio Grande do Sul (UFRGS)


Abstract: Regge theory is presently a valued tool in the investigation of the mainfeatures of soft hadronic interactions and an important guide in the search ofa fundamental theory for soft processes based upon QCD. At high energies thePomeron plays a crucial part in describing the soft interactions. In the lightof LHC data we perform a detailed analysis of proton-proton and antiproton-proton forward scattering data, and obtain extrema bounds for the soft Pomeronintercept using both eikonal and Born-level amplitudes. In our analysis we in-vestigate the effects of exponential and power-like forms for the elastic Pomeron-proton vertex. In order to improve the large b region we incorporate the nearestt-channel singularity of the Pomeron trajectory, namely the two-pion loop. Wegive predictions for proton-proton total cross section at Tevatron, LHC, andcosmic-ray energies. (email*: [email protected])

Simplified Thermal Evolution of Proto-hybrid StarsMauro Mariani*, Milva Orsaria, and Hector Vucetich

Facultad de Ciencias Astronomicas y GeofısicasUniversidad Nacional de La Plata (FCAG/UNLP)

La Plata, Argentina

Abstract: We study the possibility of a hadron-quark phase transition in theinterior of neutron stars, taking into account different schematic evolutionarystages at finite temperature. We also discuss the strange quark matter sta-bility in the quark matter phase. Furthermore, we analyze the astrophysicalproperties of hot and cold hybrid stars, considering the recent constraint onmaximum mass given by the pulsars PSR J1614-2230 and PSR J1614-2230.We obtain cold hybrid stars with maximum masses > 2MSun and analyze, ina simplified way, different stages of hot hybrid stars as a first approximationto the cooling evolution of neutron stars with quark matter cores. (email*:[email protected])

Cosmic Censorship in a Kantowsky-Sachs SpacetimeMiguel De Campos*, Patricia Carvalho, and B. Terezon

Universidade Federal de Roraima (UFRR)Boa Vista, Brazil

Abstract: The Kantowski-Sachs (KS) model presents somewhat different fea-tures from models that usually populate the Bianchi classification, i.e., the


model is resulting from the product of a sphere with a line (R3 x R), and canbe described as a spatially homogeneous, isotropic model, that does not permita simple transitive group of motions. From the cosmological point of view, theKS universe with a positive cosmological term (that the more plausible interpre-tation is considering as the vacuum energy of the all fields in the cosmic fluid)can admit an inflationary phase during which occur the isotropization process,and , naturally, the shear decays exponentially. However, if we are dealing witha cosmological model or if we treat the gravitational collapsing process, in thetruth, both studies can to be considered as the two sides of the same coin. Muchhas already been published considering cosmological KS- models, however, ourintend in this work is analyze the cosmic censorship conjecture in an anisotropiccollapsing process, with for some different contents in the material side of theEinstein field equations, with or without an interaction with a vacuum energycomponent. (email*: [email protected])

The Generalized Expression for Symmetry Energy in a Class ofNonlinear Relativistic Nuclear Models

Moises Razeira* and Cesar Zen VasconcellosUniversidade Federal do Pampa (UNIPAMPA)

Cacapava do Sul, Brazil

Abstract: The symmetry energy play an important role in nuclear astro-physics, ranging from structure of nuclei to neutron stars physics. In this workwe have derived a simple semi-analitc expression for the symmetry energy in anframe work of generalized derivative coupling model for dense nuclear matter.We have investigated the density dependence of symmetry energy for highlyasymmetric nuclear matter with explicit inclusion of the scalar isovector meson.(email*: [email protected])

Braking Indices of Pulsars Obtained in the Presence of an EffectiveForce

Nadja Simao Magalhaes*1, A.S. Okada1 and C. Frajuca21Universidade Federal de Sao Paulo - UNIFESP, Diadema, Sao Paulo, Brazil

Instituto Federal de Educacao, Ciencia e Tecnologia (IFSP)Sao Paulo, Brazil

Abstract: The theoretical determination of pulsars’ braking indices is an openproblem. In this talk we report results on this issue changing the canonicalmodel (which admits that pulsars are rotating magnetic dipoles) basically byintroducing a compensating component in the energy conservation equation ofthe system, which would correspond to an effective force that varies with thefirst power of the tangential velocity of the pulsars crust. We tested the modelusing data available as well as predicted braking index values for different stars,and we comment on the high braking index recently measured for the pulsarJ16404631. (email: [email protected])

A New Approach on Quantum GravityNilo Serpa


Faculdades Integradas Promove (ICESP)Brasılia, Brazil

Abstract: This article discusses quantum gravity through a new approach basedon a model of quantization of the spacetime. Singularity functions are appliedto the study, whose main focus is to investigate the physics in the surroundingsof supermassive bodies. The work is a continuation of the research program onquantum gravity, time machines and supergravity established by the author intwo previous publications, one in 2015 and another in 2016. This article alsoopens the way for a broader debate on gravitation, seeking to rescue a physicaldiscourse and not merely a math exercise. (email: [email protected])

Quark Matter Under Strong Magnetic Fields in Chiral QuarkModels

Norberto Scoccola*, V. Pagura, D. Gomez Dumm, and S. NogueraComission Nacional de Energıa Atomica (CNEA)

Buenos Aires, Argentina

Abstract: The influence of intense magnetic fields on the properties of quarkmatter is investigated using a SU(2)f non-local chiral quark model. (email*:[email protected])

Dimensionally Compactified Chern-Simon Theory in 5D as aGravitation Theory in 4D

Olivier Piguet*, Ivan Morales, Bruno Neves, and Zui OportoUniversidade Federal de Vicosa (UFV)

Vicosa, Brazil

Abstract: We propose a gravitation theory in 4 dimensional space-time obtainedby compacting to 4 dimensions the five dimensional topological Chern-Simonstheory with the gauge group SO(1,5) or SO(2,4) – the de Sitter or anti-de Sit-ter group of 5-dimensional space-time. In the resulting theory, torsion, whichis solution of the field equations as in any gravitation theory in the first or-der formalism, is not necessarily zero. However, a cosmological solution withzero torsion exists, which reproduces the Lambda-CDM cosmological solutionof General Relativity. Attempts to find realistic solutions with spherical sym-metry are also considered. Finally, ways of quantizing the theory are discussed.(email*: [email protected])

Stellar Structure Models of Deformed Neutron StarsOmair Zubairi* and Fridolin Weber

Department of Sciences, Wentworth Institute of Technology (WIT)Boston, USA

Abstract: Traditional stellar structure models of non-rotating neutron starswork under the assumption that these stars are perfect spheres. This assump-tion of perfect spherical symmetry is not correct if the matter inside neutronstars is described by an anisotropic model for the equation of state. Certain


classes of neutron stars such as Magnetars and neutron stars which containcolor-superconducting quark matter cores are expected to deformed makingthem oblong spheroids. In this work, we examine the stellar structure of thesedeformed neutron stars by deriving the stellar structure equations in the frame-work of general relativity. By using a non-isotropic equation of state model, wesolve these structure equations numerically in two dimensions. We calculate stel-lar properties such as masses and radii along with pressure and energy-densityprofiles and investigate any changes from standard spherical models. (email*:[email protected])

Quadrupole Mass Optimization in Very High Speed Using FEMPaulo Roberto Murger Nogueira* and Carlos Frajuca

Instituto Federal de Educaco, Ciencia e Tecnologia de Sao Paulo (IFSP)Sao Paulo, Brazil

Abstract: A experiment to measure the velocity of gravity is been planning. Inorder to achieve a reasonable signal in the detector, a very massive quadrupolemass is put to rotate at a very high rotation speed. in order to maximize thesignal, the mass much be as higher as possible. This work test mass-quadrupolegeometries in Finite Element Modeling with the goal to maximize the signal.(email*: [email protected])

On Pair Intability Supernovae Explosion and Gamma-Ray BurstsPascal Chardonnet*, A. Baranov, V. Chechetkin, A. Filina,

M. Popov And N. SmirnovaLaboratoire d’Annecy-le-Vieux de Physique Theorique

Universite Savoie Mont BlancSavoie, France

Abstract: The enigma of cosmic gamma-ray bursts is tool to understand howa star ends his life with this magnificent firework. The standard fireball sce-nario developed during many years has provided a possible explanation of thisphenomena. The aim of this presentation is simply to explore a new possibleinterpretation; by developing a coherent scenario inside the global picture ofstellar evolution, as a missing link of stellar evolution. At the basis of our sce-nario is the fact that maybe we have not fully understood how the core of apair instability supernovae explode. In such a way, we have proposed a newparadigm assuming that the core of such massive star, instead of doing a sym-metrical explosion, is completely fragmented in hot spots of burning nuclearmatter. We have tested our scenario using some observational data like GRBspectra, light curves, Amati relation and GRB-SN connection, and for each setof data we have proposed a possible physical interpretation. We ha ve also sug-gested some possible tests of this scenario by measurements at high redshift.(email*: [email protected])

Neutrinos in CosmologyPedro Cunha de Holanda



Abstract: (email: [email protected])

Thermodynamics of Nonsingular Bouncing UniversesPedro da Cunha Ferreira* and Diego Pavon

Escola de Ciencias e Tecnologia, Universidade Federal do Rio Grande do Norte(ECT/UFRN)Natal, Brazil

Abstract: Homogeneous and isotropic, nonsingular, bouncing world models aredesigned to evade the initial singularity at the beginning of the cosmic expan-sion. Here, we study the thermodynamics of the subset of these models governedby general relativity. Considering the entropy of matter and radiation and con-sidering the entropy of the apparent horizon to be proportional to its area, weargue that these models do not respect the generalized second law of thermo-dynamics, also away from the bounce. (email*: [email protected])

Tsallis Statistics and Hadronic MatterPedro Henrique Goulart Cardoso* and Debora Peres Menezes


Abstract: In this work we intend to get physical properties of quark starsusing the MIT bag model to obtain the equations of state and the Tolman-Oppenheimer-Volkoff for the profile of star. The proposal is to replace the Fermi-Dirac statistics used to describe the fermi gas in the Mit bag model, by Tsallisstatistics. We seek with this non-additive statistics, but extensive for complexsystems, get new results related to the profile of a possible quarks star andcompare them with observational data. (email*: [email protected])

Stellar Equilibrium Configurations of Compact Stars in f(R, T )Theory of Gravity

Pedro MoraesInstituto Tecnologico de Aeronautica (ITA)


Abstract: In this work we study the hydrostatic equilibrium configuration ofneutron stars and strange stars, whose fluid pressure is computed from theequations of state p = 5/3 and p = 0.28(4B), respectively, with ω and B beingconstants and ρ the energy density of the fluid. We start by deriving the hy-drostatic equilibrium equation for the f(R, T ) theory of gravity, with R and Tstanding for the Ricci scalar and trace of the energy-momentum tensor, respec-tively. Such an equation is a generalization of the one obtained from generalrelativity, and the latter can be retrieved for a certain limit of the theory. Forthe f(R, T ) = R + 2λT functional form, with λ being a constant, we find thatsome physical properties of the stars, such as pressure, energy density, massand radius, are affected when λ is changed. We show that for a fixed centralstar energy density, the mass of neutron and strange stars can increase with λ.Concerning the star radius, it increases for neutron stars and it decreases for


strange stars with the increment of λ. Thus, in f(R, T ) theory of gravity wecan push the maximum mass above the observational limits. This implies thatthe equation of state cannot be eliminated if the maximum mass within GeneralRelativity lies below the limit given by observed pulsars. DOI: 10.1103/Phys-RevD.94.024032. (email: [email protected])

The Present Status of the Pseudo-complex General RelativityPeter Otto Hess

Instituto de Ciencias Nucleares, Universidad Nacional Autonoma de Mexico(ICN/UNAM)

Mexico City, Mexico

Abstract: I will present the present status of the pseudo-complex General Rel-ativity. It will be shown that it contains many known theories with a minimallength. Retricting to its simplest form, an energy-momentum tensor is added atthe right hand side of the Einstein equations, representing a dark energy, relatedto vacuum fluctuations. We use a phenomenological ansatz for the denisty anddiscuss observable consequences. (email: [email protected])

Application of Modern Neutron Star Equations of State in theStudy of SGRs and AXPs Properties

Rafael Camargo Rodrigues de Lima*, Jaziel G. Coelho,Diego L. Caceres, Jorge A. Rueda, and Remo Ruffini

Universidade do Estado de Santa Catarina (UDESC)Florianopolis, Brazil

Abstract: We show that nine of the twenty three soft gamma repeaters (SGRs)and anomalous X-ray pulsars (AXPs), namely the 40pulsars driven by the ro-tational energy of a neutron star (NS), for which we give the possible range ofmasses. We also show that if the blackbody component in soft X-rays is due tothe surface temperature of the NS, then two more sources become explainableas rotation-powered NSs, leading to a 50the population explainable as ordinarypulsars. We show that, within these sources, we find the SGRs/AXPs withobserved radio emission as well as the ones possibly associated with supernovaremnants, reinforcing a natural explanation for these sources as ordinary pul-sars. Assuming on the other hand an alternative model in which SGR/AXPs arerotation-powered white dwarfs (WDs), we show that the entire population canbe explained within this scenario. We give tight bounds for the masses, radii,and magnetic field of the WD by requesting the gravitational and rotationalstability of the star. (email*: [email protected])

Testing Anomalous Diffusion Models for Simulation of InitialDensity Fluctuation Spectra in Hierarchical Large Scale Structure

FormationReinaldo Roberto Rosa

Laboratorio Associado de Computacao e Matematica Aplicada (LAC)Instituto Nacional de Pesquisas Espaciais (INPE)



Abstract: It is already known that structure formation was predominately atsuperhorizon scales during the inflation era and so must be treated by generalrelativity. However, in specific periods when dissipation becomes significant, theinfluence of fluctuation to structure formation is of sub-horizon scales, and canbe described by a non relativistic approximation. In this framework, the hypoth-esis of non-Gaussian stochastic processes has become important in the study ofthe structure formation in hierarchical scenarios. In this work we present the ap-plication of anomalous diffusion models (especially KPZ-equation and equivalentautomata) to simulate density fluctuation spectra in the Lambda-CDM cosmol-ogy. The models are tested in the following ways: fluctuation maps are generatedserving as initial conditions in large-scale structure formation. The anomalousdiffusion spectra are validated based on the statistical properties of voids andfilaments obtained for low redshifts (z < 1). (email: [email protected])

GRBs, Crab Nebula and Active Galactic NucleiRemo Ruffini

International Centre for Relativistic Astrophysics Network (ICRANet),Sapienza - Universit di Roma

Roma, Italy

Abstract: (email: [email protected])

The Low-temperature Astrophysical HD-cooling FunctionRenat Anasovich SultanovSt. Cloud State University

Minnesota, USA

Abstract: Energy transfer collisions between H2 and HD molecules, where H ishydrogen and D is deuterium, is of fundamental importance for the astrochem-istry of the early Universe [1] and the interstellar medium [2]. HD representsthe second most abundant primordial molecule after H2 and plays a significantrole in the cooling of the primordial gas. The abundance of deuterium is lowrelative to hydrogen, i.e. n(D)/n(H) ∼ 0.00001, however the HD/H2 ratio canbe enhanced by an approximate factor of ∼ 100 due to chemical fractionation,for example, through the following chemical reactions: H2 +D+ → HD +H+

or H2 +D → HD +H. It has been shown, that in the framework of the stan-dard cosmological model the radiation temperature is higher than the mattertemperature and molecules become a heating source for the gas. At higher tem-peratures H2 molecules dominate the heating, however HD molecules dominatethe kinetic process at lower temperatures [1]. In addition, the HD molecule isespecially important due to its permanent dipole moment and lower rotationalconstant. It makes the molecule to be an efficient coolant at lower temperatures:T < 100K. Knowledge of the rotational-vibrational excitation and de-excitationthermal rate constants in the molecular HD + H/H2 low energy collisions is ofsignificant importance in understanding and modeling of the energy balancewithin primordial gas. Therefore, in this work we carry out a pure quantum-mechanical calculation of the non-reactive scattering processes HD + H2 andHD+H. We compute their rotational energy transfer cross-sections and thermalrate coefficients at low temperatures of astrophysical interest. The most recent


H3 and H4 potential energy surfaces have been used with some important modi-fications because of the symmetry break in the target - HD instead of H2 [3]. Aquantum-mechanical close-coupling approach has been applied [3]. After thesecareful calculations, one can carry out a new estimation of the astrophysicalHD-cooling function at different temperatures and astrophysical conditions. [1]A. Dalgarno and R. McCray, 1972, Ann. Rev. Astron. Astrophys. 10, 375. [2]C. M. Coppola, L. Lodi and J. Tennyson 2011, Mon. Not. R. Astron. Soc.,415, 487. [3] R.A. Sultanov, D. Guster, and S.K. Adhikari, 2016, J. Phys. B:At. Mol. Opt. Phys., 49, 015203. (email: [email protected])

Chiral Symmetry Restoration for Quark Matter with a ChiralImbalance: agreement with lattice results

Ricardo L. S. Farias*, D. C. Duarte, G. Krein, and R. O. RamosUniversidade Federal de Santa Maria (UFSM)

Santa Maria, Brazil

Abstract: There has been recently an increased interest in the study of how achiral imbalance of right-handed and left-handed quarks can influence the phasediagram of quantum chromodynamics (QCD). There are many good reasons forthis interest. For instance, the nontrivial nature of the vacuum of non-Abeliangauge theories in general, and of QCD in particular, allows for the existenceof topological solutions like instantons and sphalerons. A chirality imbalanceis expected to occur in event-by-event in heavy-ion collision experiments (Cand CP violations). When these effects are associated with a magnetic field,they can induce an electric current due to the chirality imbalance, an effectdubbed the chiral magnetic effect (CME) in the literature. The effects of achiral imbalance in the phase diagram of QCD can be studied in the grandcanonical ensemble by the introduction of a chiral chemical potential µ5 in theQCD Lagrangian density. It is intriguing that models that have been verysuccessful in describing many features predicted by universality arguments andlattice simulations for the chiral transition in QCD at nonzero T and µ, havedifficulties in reproducing, even at a qualitative level, recent lattice results forthe chiral critical transition temperature Tc at finite µ5. We show how a simplescheme of rewriting a divergent momentum integral can reconcile conflictingresults obtained for the chiral critical transition line between some effectivemodels for Quantum Chromodynamics (QCD) and recent lattice results, whenin the presence of a chiral imbalance. Our results show an increasing criticaltemperature for chiral symmetry restoration as a function of the chiral chemicalpotential µ5. This result is consistent with recent lattice results and also withsome other more involved analytical and numerical non-perturbative studies.(email*: [email protected])

Neutral Pion Pole Mass Calculation in a Strong Magnetic Field:lattice QCD versus NJL model

Ricardo L. S. Farias*1,2, Sidney S. Avancini3, Marcus Benghi Pinto3,William R. Tavares1, and Varese S. Timoteo1,4

1 Departamento de Fısica, Universidade Federal de Santa Maria, 97105-900Santa Maria, RS, Brazil


2 Physics Department, Kent State University, Kent, OH 44242, USA3 Departamento de Fısica, Universidade Federal de Santa Catarina, 88040-900

Florianopolis, Santa Catarina, Brazil4 Grupo de Optica e Modelagem Numerica (GOMNI), Faculdade deTecnologia, Universidade Estadual de Campinas - UNICAMP, Brazil

Abstract: The π0 neutral meson pole mass is calculated in a strongly magne-tized medium using the SU(2) Nambu-Jona-Lasinio model within the randomphase approximation (RPA) at zero temperature and zero baryonic density. Weemploy a magnetic field dependent coupling G(eB) fitted to reproduce latticeQCD results for the quark condensates. Divergent quantities are handled witha magnetic field independent regularization scheme in order to avoid unphysicaloscillations. A comparison between the running and the fixed couplings revealsthat the former produces results much closer to the predictions from recentlattice calculations. In particular, we find that the π0 meson mass systemati-cally decreases when the magnetic field increases while the scalar mass remainsalmost constant. We also investigate how the magnetic background influencesother mesonic properties such as fπ0

and gπ0qq. The results obtained in this workseem to indicate that the use of a running coupling within a robust theoreticalframework, such as the RPA-MFIR, turns the simple NJL into a useful tool toinvestigate magnetized quark matter. (email*: [email protected])

Exploring Hot QCD in Magnetic FieldsRicardo L. S. Farias*1,2, Varese S. Timoteo3, Sidney S. Avancini4, Marcus

Benghi Pinto4, and Gastao I. Krein51 Departamento de Fısica, Universidade Federal de Santa Maria, 97105-900

Santa Maria, RS, Brazil2 Physics Department, Kent State University, Kent, OH 44242, USA3 Grupo de Optica e Modelagem Numerica (GOMNI), Faculdade deTecnologia, Universidade Estadual de Campinas - UNICAMP, Brazil

4 Departamento de Fısica, Universidade Federal de Santa Catarina, 88040-900Florianopolis, Santa Catarina, Brazil

5 Instituto de Fısica Teorica, Universidade Estadual Paulista, Rua Dr. BentoTeobaldo Ferraz, 271 - Bloco II, de Sao Paulo

Sao Paulo, Brazil

Abstract: The investigation of the effects produced by a magnetic field in thephase diagram of strongly interacting matter became a subject of great interestin recent years. The recent motivation stems mainly from the fact that strongmagnetic fields may be produced in noncentral heavy-ion collisions. Strong mag-netic fields are also present in magnetars and might have played an importantrole in the physics of the early universe. At zero temperature, the great major-ity of effective models for Quantum Chromodynamics (QCD) are in agreementwith respect to the occurrence of the phenomenon of magnetic catalysis (MC),which refers to the increase of the chiral order parameter represented by the(light) quark condensates with the strength of the magnetic field. On the otherhand, at finite temperature such models fail to predict the inverse magneticcatalysis (IMC), an effect discovered by lattice QCD (LQCD) simulations, inthat the pseudo-critical temperature for chiral symmetry restoration decreasesas B increases. In this work we will present recent results where we advocate


that the phenomenon of inverse magnetic catalysis of chiral symmetry in QCDpredicted by lattice simulations can be reproduced within the Nambu–Jona-Lasinio model if the coupling G of the model decreases with the strength Bof the magnetic field and temperature T . The thermo-magnetic dependenceof G(B, T ) is obtained by fitting recent lattice QCD predictions for the chiraltransition order parameter. Different thermodynamic quantities of magnetizedquark matter evaluated with a G(B, T ) are compared with the ones obtained atconstant coupling G. The model with a G(B, T ) predicts a more dramatic chiraltransition as the field intensity increases. In addition, the pressure and magne-tization always increase with B for a given temperature. Being parametrizedby four magnetic field dependent coefficients and having a rather simple expo-nential thermal dependence our accurate ansatz for the running coupling can beeasily implemented to improve typical model applications to magnetized quarkmatter. (email*: [email protected])

Statistical Evidence of the Two Neutrinos Bursts from SN1987ARodolfo Valentim*, J.E. Horvath and E.M. Rangel

Instituto de Astronomia, Geofısica e Ciencias Atmosfericas, Universidade deSao Paulo (IAG/USP)

Sao Paulo, Brazil

Abstract: The explosion of SN1987A into Giant Magellanic Cloud was an ex-traordinary event because it was observed in the real time for different neu-trino experiments. It was observed about twenty five events in the detectors:Kamiokande II (KII) ∼ 12, Irvine-Michigan-Brookhaven (IMB) ∼ 8 e Baksan∼ 5. Neutrinos have an important play on Neutron Star (NS) newborn cool-ing (∼ 99% of the collapase energy is lost when neutrinos are issued in thefirst seconds). This work is developed through Bayesian Statistics tools (mainlyBayesian Information Criterion - BIC) and we used likelihood function for esti-mating the emission temperature of neutrinos (Tν) and the neutrinosphere radii(Rν) by two emission models: 1o exponential cooling model with three param-eters and 2o two temperatures model with four parameters. The first modelassumes a cooling mechanism with an exponential decay law temperature andassumes the existence of only one burst neutrino. The second model, with twodifferent temperatures suggests the existence of two bursts when the NS born.Comparing these different models, the BIC showed a strong evidence in favorof the second model (lnBij > 5.0). This outcome suggests the existence ofthe two neutrinos bursts at the moment of the supernovae explosion. (email*:[email protected])

Existence of Cold Quark Matter in Nature: models andobservations

Rodrigo Alvares de Souza* and Jorge HorvathInstituto de Astronomia, Geofısica e Ciencias Atmosfericas, Universidade de

Sao Paulo (IAG/USP)Sao Paulo, Brazil

Abstract: The main goal of this work is the study of cold quark matter inneutron stars from phase transitions of hadronic matter to quark matter. To


describe the hadronic phase in this work we studied the SWRDP model, whichconsiders hyperons and the effects of many-body forces simulated by the nonlin-ear selfcoupling and the meson-meson contributions. The matter of quarks wasdescribed by two approaches: the QCD Mean Field Theory (MFTQCD) andQCD Infrared Extension (QCDIRE). The approach used to make the connec-tion between hadronic matter and the cold quark matter was a first order phasetransition using the Maxwell construction. Next, the hybrid state equationswere integrated using the Tolman-Oppenheimer-Volkoff equations and obtainedmaximum masses for some sets of parameters that are in agreement with obser-vations of pulsars PSR J1614-2230 (M = 1.97± 0.04M) and PSR J0348+0432(M = 2.01± 0.04M). (email*: [email protected])

Strange Stars with Anisotropy Coupled to CompactnessRodrigo Francisco dos Santos* and Luis Gustavo Almeida

Universidade Federal Fluminense (UFF)Niteroi, Brazil

Abstract: We solve the TOV equations for the EOS of strange stars, wherewe adopted anisotropy coupled with compactness. This coupling points to ananisotropy with a different source of the usual, where normally we work withanisotropy generated by the presence of electric charge on the star. In this caseour intention is to start studying the influence of the cosmological constant incompact objects. Our results point to the increase of mass in star as a result ofassuming anisotropy coupled with compactness. This result is consistent withrecent experimental results.(email*: [email protected])

The Cherenkov Telescope Array: unveiling the gamma rayUniverse

Rodrigo NemmenInstituto de Astronomia, Geofısica e Ciencias Atmosfericas, Universidade de

Sao Paulo (IAG/USP)Sao Paulo

on behalf of the Cherenkov Telescope Array (CTA) Consortium

Abstract: Gamma-ray astronomy allows synergies between Astrophysics, Par-ticle Physics and Cosmology. The Cherenkov Telescope Array (CTA) is aninternational initiative to build the next-generation ground-based gamma-rayobservatory which will be composed of hundreds of Cherenkov telescopes andwill have a factor of 5-10 improvement in sensitivity in the 100-GeV to 10-TeVrange, with a large energy coverage from a few tens of GeV to a few hundredsof TeV. CTA will consist of two arrays — one in the Canarias Island in theNorth and another in Chile in the South Hemisphere — and will provide adeep insight into the non-thermal high-energy Universe and its particle accel-erators. In this talk, I will briefly present the major design concept of CTA,its vast science case and the Brazilian participation in the consortium. ([email protected])


Anisotropies detected by Pierre Auger Observatory in theUltra-High Energy Cosmic Rays Sky

Rogerio M. de AlmeidaUniversidade Federal Fluminense (UFF)

Niteroi, BrazilThe Pierre Auger Collaboration

Abstract: The study of anisotropies in the flux of high-energy cosmic rays car-ries major clues to understanding their origin. The Pierre Auger Collaboration,in operation since 2004, is the largest cosmic ray observatory in the world. Wereview their recent results related to anisotropies in the arrival directions ofultra-high energy cosmic rays. We present searches for dipolar and quadrupolaranisotropies in different energy ranges spanning four orders of magnitude. Forthe highest energy cosmic rays, with energies above the predicted GZK cutoff,we present an update of the search for correlations between their arrival direc-tions and the positions of active galactic nuclei from the Veron-Cetty and Veroncatalog. We also examine the correlation of arrival directions with other popu-lations of nearby extragalactic objects. Finally, we report the results of a blindsearch for localized excess fluxes and for self-clustering of arrival directions atangular scales up to 30 degrees and for different energy thresholds between 40EeV and 80 EeV. (email: [email protected])

White Dwarfs Pulsar as Sources of Ultra-high Cosmic RaysRonaldo Vieira Lobato*, Laura Paulucci, and Manuel Malheiro.


Abstract: The origin of highest energy cosmic rays still remains a mystery inAstrophysics. In this work we consider the Soft Gamma Repeaters (SGRs)and Anomalous X-ray Pulsars (AXPs) as possible sources of ultra-high cosmicrays. These stars described as white dwarfs pulsars can achieved large electricpotential differences in their surface and accelerate particles up to Lorentz fac-tors γ ∼ 1010 . Pulsars offer favorable sites for the injection of electrons andheavy nuclei, and accelerate them to ultrahigh energies. Once accelerated inthe pulsar this particles can escape from the magnetosphere and produce theradiation observed. Here, we discuss the possibility of SGRs/AXPs as whitedwarf pulsars to be possible sources of ultra-high energetic photons. (email*:[email protected])

Many-body Forces in the Equation of State of Magnetized NeutronStars

Rosana de Oliveira Gomes*, B. Franzon, V. Dexheimer,S. Schramm, and C.A.Z. Vasconcellos


Abstract: The observation of compact objects with surface magnetic fields asstrong as 1014 − 1015 G, denominated magnetars, has drawn attention to thestudy of the effects of strong magnetic fields on nuclear matter and compact


stars observational properties. In the interior of magnetars, the magnetic fieldsare expected to be even stronger, and might reach values up to 1019 G. Inthis work, we study the effects of strong magnetic fields on the equation ofstate and structure of neutron stars. We describe nuclear matter inside starsin a new relativistic mean field formalism that takes many-body forces intoaccount, by means of a field dependence of the nuclear interaction couplingconstants. Assuming that matter is at zero temperature, charge neutral, beta-equilibrated and populated by the baryonic octet, electrons and muons, weexplore the parameters space of the model in order to describe the nuclear matterproperties at saturation, as well as massive hyperon stars. Also, in the context ofthe so called hyperon puzzle, we investigate the role of hyperon potentials in themass-radius relation and population of hyperon stars, by solving the Tolman-Oppenheimer-Volkoff (TOV) equations. The presence of the magnetic fieldsgenerates a Landau quantization on the energy levels of the charged particlesand also an anisotropy in the rocomponents of the energy-momentum tens. Wealso calculate the effects of the anomalous magnetic moment of the particles onthe energy levels of all particles, including the uncharged ones, and show that itincreases the magnetization of the matter. Finally, we introduce the magneticfields in the strutucture of stars by solving the Einstein-Maxwell equations self-consistently. This solutions lead to stationary and axi-symmetric stellar models,in which a poloidal magnetic field is assumed. Hence, the matter is consideredto be under a static density dependent magnetic field, reaching intensities of theorder of 1018 G at the center of the stars. We conclude that magnetic fields affectsignificantly the particles population of the stars, but only the effects on thestrucuture of stars have strong influence on the global properties, as maximummasses and deformation, of these objects. (email: [email protected])

Bayesian Inference Applied to Pulsars’ ModelsRubens de Melo Marinho Junior*, Nadja S. Magalhaes, Heitor

Oliveira, Marcio E.S. Alves, Jaziel G. Coelho, and Rodolfo ValentimInstituto Tecnologico de Aeronautica (ITA)


Abstract: There are strong evidences that pulsars are rotating magnetized neu-tron stars emitting electromagnetic radiation in a wide range of wavelengths.The variation of the angular frequency is an observational evidence that theirrotation energy decreases. However, it is well known that the canonical modelfor magnetic dipole radiation cannot precisely explain the energy loss. There isa variety of models trying to explain the phenomenon, such as the energy lossdue to the emission of gravitational radiation, quantum vacuum friction andinteraction of the magnetic field with the plasma surrounding the star, and/oralso the variation of the magnetic field, angle inclination and the moment ofinertia, etc. Moreover, the equations that describe the phenomenon are func-tions of the mass-radius relation of the neutron star and so far it is not knownwhich Equation of State (EoS) for nuclear matter should be used to describe thestar’s interior. The goal of this work is to apply Bayesian inference through BIC(Bayesian Information Criterion) to select among different theoretical modelsand EoS those that better fit known pulsar data for the rate of decrease of an-gular velocity versus the angular velocity itself. After selecting the model, we


also find the posterior distribution and the best fit for some relevant parametersof the pulsar like the mass and the magnetic field. (email*: [email protected])

Compact objects in a Brana Generalised ModelSamuel Isidoro Dos Santos JUnior

Instituto Tecnologico de Aeronautica - ITA, Sao Jose dos Campos, Brazil

Abstract: Great as are the efforts in the study of the composition and inter-nal structure of compact stars, the absolute ground state of matter is still anopen question. The analysis of matter at high densities in the universe has asone of its fronts the characterization of gravitational waves emitted by binarysystems with compact objects. The aim of this study is to characterize thegravitational wave polarization states in f(R,T) theories, in which the gravita-tional part of the action depends on a generic function of R, the Ricci scalar,and T, the trace of the energy-momentum tensor. This characterization, be-sides contributing to the study of matter at high densities can be supported byexperiments as Advanced LIGO, which will soon come into operation. More-over, although the scope of the f(R,T) theories, we propose to obtain Tolman-Oppenheimer-Volkoff equations as well as their solutions in order to identifyrelevant physical quantities in the study of superdense matter in the universe.(email: [email protected])

Dark Matter Search with the ATLAS DetectorSergey Burdin University of Liverpool

Liverpool, United Kingdomfor ATLAS Collaboration (Large Hadron Collider (LHC))

Abstract: Dark Matter comprises approximately 27% of the universe yet littleis known about its properties. Dark matter particles, if produced by the LHC,will leave a distinct signature of significant missing transverse energy (MET).Recent results from ATLAS utilising the MET signature found in associationwith a variety of probes will be presented. (email: [email protected])

TitleSergio Jose Barbosa Duarte

Centro Brasileiro de Pesquisas Fısicas (CBPF)Rio de Janeiro, Brazil

Abstract: (email: sbd@cbpf)

White Dwarf StarsS.O. Kepler


Abstract: We study the white dwarf mass and distance distribution, and thediscovery of a normal mass white but devoided of any H,He and C. (email:[email protected])


The pT -distribution to the exclusive photoproduction of J/ψ andψ(2S) in pp and AA collisions at LHC energiesSony Martins* and Maria Beatriz Gay DucatiUniversidade Federal do Rio Grande do Sul (UFRGS)


Abstract: The exclusive photoproduction of heavy vector mesons allows usto analyse hard-diffractive process from perturbative quantum chromodynamics(QCD). In other words, we have the opportunity to investigate the QCD natureof the pomeron, a fundamental object of physical diffractive, described by linearevolution equation BFKL. At high energy, it is expected a transition between theregime described by the linear dynamics, governed by DGLAP and BFKL, andthe non-linear dynamics, where the recombination of partons (mainly gluons)becomes important. In this last case, the phase-space parton density reaches alimit in the hadron wave function, characterizing the saturation phenomenum.In this work, the theoretical framework considered in the analysis is the light-cone dipole formalism, where the photon-target interaction amplitude can bewritten as a convolution between the overlap of the photon-meson wave functionsand the dipole-target cross section. Using different phenomenological models,we calculate the transverse momentum distribution in central rapidity for themesons J/psi and psi(2S) in ultra-peripheral collisions proton-proton and Lead-Lead at 13 TeV and 5.5 TeV, respectively. (email*: [email protected])

Isospin Effects in the Neutron Star CrustStefan Schramm* and Rana NandiFrankfurt Institute for Advanced Studies

Frankfurt Am main, Germany

Abstract: The properties of the neutron star crust are crucially important formany physical processes occurring in the star. For instance, the crustal trans-port coefficients define the temperature evolution of accreting stars after bursts,which can be compared to observation. Furthermore, the structure of the innercrust can modify the neutrino transport through the matter considerably, sig-nificantly impacting the dynamics of supernova explosions. As the neutron starenvironment is highly isospin asymmetric, we perform a study of the inner crust,and in particular, the dependence of the pasta phase on the isospin properties ofthe nuclear interactions. To this end we developed an efficient computer code tosimulate the inner and outer crust using molecular dynamics techniques. I willpresent numerical results with regard to the pasta phase, varying the isospinparameters of the interactions. Results with regard to the nature of the tran-sition from inner crust to the neutron star core will be given and discussed aswell. (email*: [email protected])

Feeding the “Monster: supermassive black holes at the center ofgalaxies

Thaisa Storchi BergmannUniversidade Federal do Rio Grande do Sul (UFRGS)



Abstract: Supermassive black holes seem to be present in the nuclei of all mas-sive galaxies, evolving with them since the first billion years of age of the Uni-verse. This co-evolution occurs via the feeding and feedback processes of thesupermassive black hole that can be observed when the galaxy becomes “activevia capture of mass by the black hole. In my talk, I will discuss these processesand the constraints posed to them by recent observations of the inner region ofgalaxies (1-3 thousand light years radius) and the resulting implications for theevolution of the Universe. (email: [email protected]). About the speaker: ThaisaStorchi Bergmann is a full professor at Instituto de Fsica, IF-UFRGS, PortoAlegre, RS, Brasil, where she is the head of the astrophysics research group.She obtained her PhD at IF-UFRGS and did post-doctoral studies at the Uni-versity of Maryland, Space Telescope Science Institute, Rochester Institute ofTechnology and Harvard Smithsonian Center for Astrophysics, in the US. Sheis member of the Brazilian Academy of Sciences, of the Academy of Sciencesof the Developing World (TWAS) and in 2015 received the L’Oreal/UNESCOaward For Women in Science for her contribution to science in the study of theco-evolution of Supermassive Black Holes and galaxies.

Dark Spinor Field in Inflationary CosmologyThiago Vinicius Moreira Guimaraes* and Saulo Henrique Pereira

Universidade Estadual Paulista Julio de Mesquita FilhoSao Paulo, Brazil

Abstract: The theory of inflation was introduced by Alan Guth as a necessary in-gredient at the very early universe and then developed into a full working modelby Linde, Albrecht and Eteinhardt [1], and it remains the leading paradigm forthe very early universe. It naturally solves the cosmological flatness problem,absence of magnetic monopoles, horizons problem and also is consistent withhigh precision measurements of the cosmic microwave background radiation.Numerous models of inflation have been proposed in the literature, each addingnew features to the predictions of a scale invariant spectrum derived from single-field slow-roll inflation. Structure formation must also be consistent with theinflation theory. In the present work we analyze a model in which the infla-tion is not driven by a standard scalar-field, as currently proposed by most ofmodels. The analysis was carried out by considering that inflation is due to adark spinor field [2], acting something like a scalar field, but with a much morerich structure. More precisely, we show that a new class of dark spinor field incurved background with torsion is a viable alternative model for scalar driveninflation and leads to a slow-roll parameter very similar to the ones of the single-scalar-field models. Moreover, the solutions for the new inflaton field and forthe scale factor evolution have the expected behavior and can also predict theexpected mass for the inflaton, under some considerations. The numerical anal-ysis for different potentials shows a good agreement with the standard modelof inflation, which makes dark spinors as a good candidate to the inflaton field.(email*: [email protected])

The 4MOST Spectroscopic SurveyThomas Boller


Max-Planck-Institut fur Extraterrestrische Physik (MPE)Garching, Germany

Abstract: I present the science goals expected from the upcoming 4MOST spec-troscopic mission, covering tens of Millions GAIA and Millions of eROSITAAGNs and Clusters with the first light expected in 2020. The survey strategyand optimization based on intensive simulations we are presently carrying outwill also be discussed. (email [email protected])

Optimization of High Sensitivity Parametric Transducers for theGravitational Wave Detector “Mario Schenberg

Vincenzo Liccardo*Instituto Tecnologico de Aeronautica (ITA)

Elvis Ferreira, Rogeiro Oliveira, and Odylio AguiarInstituto Nacional de Pesquisas Espaciais (INPE)


Abstract: Parametric transducers may be used to monitor vibrational modes ofresonant-mass Gravitational Wave (GW) detectors. This work focuses on thedevelopment and optimization of electromechanical transducers for the BrazilianGW detector “Mario Schenberg. We present the design and preliminary resultsfor the optimization process of the last generation of the Schenberg paramet-ric transduction system. Thanks to the results obtained from the last run oftests, improvements for the transduction system will be planned and performedin order to make the detector suitable for the searching of GW signals. Theaim would be to obtain information about the direction and polarization ofwaves produced by astrophysical sources in the frequency bands of the sphericaldetector resonant modes. (email*: [email protected])

Minkowski Space Approch to the Relativistic Bound StateSpectrum

Vitor Fernando Gigante de Paiva*, Cristian Gutierrez, TobiasFrederico, Giovanni Salme, Michelle Viviani, and Lauro Tomio


Abstract: The Nakanishi integral representation of the Bethe-Salpeter ampli-tude is used in order to derive a workable framework for bound states, solutionsof the homogeneous Bethe-Salpeter Equation, in Minkowski space. The projec-tion onto the null-plane of the homogeneous Bethe-Salpeter Equation is usedto derive an equation for the Nakanishi weight function for bound states. Westudy the bound state of two spinless bosons with the interaction given by anexchanging scalar bosons in ladder+cross-ladder approximation, used to obtainthe spectrum and structure of the excited states. The unique feature of themethod is to access the valence light-front wave function. Its three-dimensionalstructure is explored in detail for the ground and excited states, by calculatingthe valence momentum distribution amplitude and the impact parameter spacerepresentation of the valence state. Resorting to the analytic structure of theNakanishi integral representation for the valence wave function, we analysed


the equality between the transverse momentum amplitudes computed withinMinkowski and Euclidean frameworks, and the leading exponential fall-off ap-pearing in the impact parameter space wave function was derived. (email*:[email protected])

Preferred Axis in CosmologyWen Zhao* and Larissa Santos

University of Science and Technology of China (USTC)Hefei, China

Abstract: The foundation of modern cosmology relies on the so-called cosmolog-ical principle which states a homogeneous and isotropic distribution of matterin the universe on the large scale. However, recent observations, such as thetemperature anisotropy of cosmic microwave background (CMB) radiation, themotion of galaxies in the universe, the polarization of quasars and the accel-eration of the cosmic expansion, indicate preferred directions of the sky. Ifthese directions have a cosmological origin, the cosmological principle would beviolated, and modern cosmology should be reconsidered. In this paper, by con-sidering the preferred axis in the CMB parity violation, we find that it coincidewith the preferred axes in CMB quadrupole and CMB octopole, and they allalign with the direction of the CMB kinematic dipole. In addition, the preferreddirections in the velocity flows, quasar alignmen, anisotropy of the cosmic ac-celeration, the handedness of spiral galaxies, and the angular distribution of thefine-structure constant are also claimed to be aligned with the CMB kinematicdipole. Since CMB dipole was confirmed to be caused by the motion of our localgroup of galaxies relative to the reference frame of the CMB, the coincidence ofall these preferred directions hits that these anomalies have a common origin,which is not cosmological or due to a gravitational effect. The systematical orcontaminative errors in observation or in data analysis, which can be directlyrelated to the motion of our local group of galaxies, can play an important rolein explaining the anomalies. (email*: [email protected])


List of Participants

1. ABRAAO JESSE CAPISTRANO DE SOUZA - Universidade Federal daIntegracao Latino Americana - UNILA, Foz do Iguacu, Brazil

2. ADAM SMITH GONTIJO BRITO DE ASSIS - Instituto Nacional dePesquisas Espaciais -INPE, Sao Jose dos Campos, Brazil

3. AHMAD A. HUJEIRAT - Interdisciplinary Center for Scientific Comput-ing - IWR, Universitat Heidelberg, Heildelberg, Germany

4. ALBERT LAZZARINILIGO Laboratory, California Institute of Technology, California, EUA

5. ALCIDES GARAT - Universidad de la Republica - UdelaR, Montevideo,Uruguay

6. ALEXANDER LUNKES DOS SANTOS - Instituto Federal Farroupilha -IFF, Campus Sao Borja, Brazil

7. ANDRE CODECO DOS SANTOS - Universidade Federal do Rio de Janeiro- UFRJ, Rio de Janeiro, Brazil

8. AURORAMARIA PEREZMARTINEZ - Instituto de Cibernetica Matematicay Fısica - ICIMAF, Havana, Cuba

9. BARBARA CELI BRAGA CAMARGO - Faculdade de Engenharia deGuaratingueta, Universidade Estadual Paulista - FEG/UNESP, Guaratingueta,Brazil

10. BIANCA PEIXOTO GOTTFRIED - Instituto Federal Farroupilha - IFF,Campus Sao Borja, Brazil

11. BRUNA CESIRA FOLADOR - Universidade Federal do Rio Grande doSul - UFRGS, Porto Alegre, Brazil

12. CARLOS FRAJUCA - Universidade de Sao Paulo - USP, Sao Paulo, Brazil

13. CESAR AUGUSTO ZEN VASCONCELLOS - Universidade Federal doRio Grande do Sul - UFRGS, Porto Alegre, Brazil

14. CLEBSON ABATI GRAEFF - Universidade Tecnologica Federal do Parana,Campus Pato Branco - UTFPR-PR; Universidade Federal de Santa Cata-rina - UFSC, Florianopolis, Brazil

15. CLEMENT STAHL - International Center for Relativistic AstrophysicsNetwork - ICRANet, Pescara, Roma, Italy

16. CRISTIAN GIOVANNY BERNAL - Universidade Federal do Rio Grande- FURG, Rio Grande, Brazil

17. CRISTIANO BRENNER MARIOTTO - Universidade Federal do RioGrande - FURG, Rio Grande, Brazil

18. DANIEL CASTRO ROMAO - Universidade Federal de Santa Catarina -UFSC, Florianopolis, Brazil


19. DANIEL COPPEDE - Instituto Federal de Educacao, Cincia e Tecnologiade Sao Paulo - IFSP, Sao Paulo, Brazil

20. DANIEL ALBERTOGOMEZ DUMM - Universidad Nacional de La Plata,Buenos Aires, Argentina

21. DANIEL TAVARES DA SILVA - Universidade Federal de Pelotas - UF-PEL, Pelotas, Brazil

22. DIMITER HADJIMICHEF - Universidade Federal do Rio Grande do Sul- UFRGS, Porto Alegre, Brazil

23. DYANA CRISTINE DUARTE - Universidade Federal de Santa Maria -UFSM, Santa Maria, Brazil

24. EDIVALDO MOURA SANTOS - Universidade de Sao Paulo - USP, SaoPaulo, Brazil

25. EDUARDO SANTOS DA VEIGA - Universidade Federal de Pelotas -UFPEL, Pelotas, Brazil

26. EDSON OTONIEL DA SILVA - Instituto Tecnologico de Aeronautica -ITA, Sao Jose dos Campos, Brazil

27. ELVIS CAMILO FERREIRA - Instituto Nacional de Pesquisas Espaciais- INPE, Sao Jose dos Campos, Brazil

28. EMERSON GUSTAVO DE SOUZA LUNA - Universidade Federal do RioGrande do Sul - UFRGS, Porto Alegre, Brazil

29. ERNESTO KEMP - Universidade de Campinas - UNICAMP, Campinas,Brazil

30. EVERTON MURILO CARVALHO DE ABREU - Universidade FederalRural do Rio de Janeiro - UFRRJ, Rio de Janeiro, Brazil

31. FABRICIO TRONCO DALMOLIN - Universidade Tecnologica Federal doParana - UTFPR, Curitiba, Brasil

32. FREDERICO FETTER GOMES - Universidade Federal do Rio Grandedo Sul - UFRGS, Porto Alegre, Brazil

33. FRIDOLIN WEBER - San Diego State University - SDSU, San Diego,USA

34. GABRIEL BORDERESMOTTA - Faculdade de Engenharia de Guaratingueta,Universidade Estadual Paulista - FEG/UNESP, Guaratingueta, Brazil

35. GEANDERSON ARAUJO CARVALHO - Instituto Tecnologico de Aeronautica- ITA, Sao Jose dos Campos, Sao Paulo, Brazil

36. GERMAN MALFATTI - Facultad de Ciencias Astronomicas y Geofısicas,Universidad Nacional de La Plata - FCAG/UNLP, La Plata, Argentina

37. GIBRAN HENRIQUE DE SOUZA - Universidade Estadual de Campinas- UNICAMP, Campinas, Brazil


38. GLAUBER SAMPAIO DOS SANTOS - Universidade Federal do RioGrande do Sul - UFRGS, Porto Alegre, Brazil

39. GUILHERME GONCALVES FERRARI - Universidade Federal do RioGrande do Sul - UFRGS, Porto Alegre, Brazil

40. GUILHERME LORENZATTO VOLKMER - Universidade Federal do RioGrande do Sul - UFRGS, Porto Alegre, Brazil

41. GUSTAVO A. CONTRERA - Universidad Nacional de La Plata - UNLP,La Plata, Argentina

42. HEITOROLIVEIRA DEOLIVEIRA - Instituto Tecnologico de Aeronautica- ITA, Sao Jose dos Campos, Brazil

43. HELIO TAKAI - Brookhaven National Laboratory - BNL, Upton, NewYork, EUA

44. HELIO TEIXEIRA COELHO - Academia Pernambucana de Ciencias -APC, Recife, Brazil

45. HENRIQUE LINARES - Instituto Federal de Educacao, Ciencia e Tec-nologia de Sao Paulo - IFSP, Brazil

46. HERCULES B. RODRIGUES - Universidade Federal de Pelotas - UFPEL,Pelotas, Brazil

47. HERMANO VELTEN - Universidade Federal do Espırito Santo - UFES,Vitoria, Brazil

48. HORACIO ALBERTO DOTTORI - Universidade Federal do Rio Grandedo Sul - UFRGS, Porto Alegre, Brazil

49. IVANA DE FREITAS CUNHA - Instituto Tecnologico de Aeronautica -ITA, Sao Jose dos Campos, Brazil

50. JAMES G. O’BRIEN - Wentworth Institute of Technology - WIT, Boston,USA

51. JOAO BRAGA - Instituto Tecnologico de Aeronautica (ITA), Sao Josedos Campos, Brazil

52. JHON ANDERSSON ROSERO GIL - Universidade Estadual de Camp-inas - UNICAMP, Campinas, Brazil

53. JONAS PEDRO PEREIRA -Universidade Federal do ABC, Santo Andre,Brazil

54. JORGE ERNESTO HORVATH - Instituto de Astronomia, Geofısica eCiencias Atmosfericas, Universidade de Sao Paulo - IAG/USP, Sao Paulo,Brazil

55. JORGE HENRIQUE DE ALVARENGA NOGUEIRA - Instituto Tec-nologico de Aeronautica - ITA, Sao Jose dos Campos, Brazil


56. JOSE ANTONIO DE FREITAS PACHECO - Observatoire de la Coted’Azur - OCA, Nice, France

57. JOSE CARLOS TEIXEIRA DE OLIVEIRA - Universidade Federal deRoraima - UFRR, Boa Vista, Brazil

58. JUSTIN ALBERT - University of Victoria, Victoria, Canada

59. KAUAN DALFOVO MARQUEZ - Universidade Federal de Santa Cata-rina - UFSC, Florianopolis, Brazil

60. LARISSA CARLOS DE OLIVEIRA SANTOS - University of Science andTechnology of China - USTC, Hefei, China

61. LAURA PAULUCCI - Universidade Federal do ABC - UFABC, SantoAndre, Brazil

62. LILIAN DE ARAUJO FERRAO - Instituto Tecnologico da Aeronautica- ITA, Sao Jose dos Campos, Brazil

63. LUIS GUSTAVO DE ALMEIDA - Universidade Federal do Acre - UFC,Rio Branco, Brazil

64. LUIS JURACY RANGEL LEMOS - Universidade Federal do Tocantins -UFT, Palmas, Brazil

65. LUIZ GARCIA DE ANDRADE - Universidade do Estado do Rio deJaneiro - UERJ, Rio de Janeiro, Brazil

66. MAGNO VALERIO TRINDADE MACHADO - Universidade Federal doRio Grande do Sul - UFRGS, Porto Alegre, Brazil

67. MAIRON MELO MACHADO - Instituto Federal de Educacao, Ciencia eTecnologia Farroupilha - IFF, Campus Sao Borja, Brazil

68. MANUEL MAXIMO BASTOS MALHEIRO DE OLIVEIRA - InstitutoTecnologico da Aeronautica - ITA, Sao Jose dos Campos, Brazil

69. MARCELLO DALLAGNOL ALLOY - Universidade Federal de SantaCatarina - UFSC, Florianopolis, Brazil

70. MARCIO EDUARDO DA SILVA ALVES - Instituto de Ciencia e Tec-nologia, Universidade Estadual Paulista - ICT/UNESP, Sao Paulo, Brazil

71. MARCIO GUILHERME BRONZATO DE AVELLAR - Institute for The-oretical Physics, J. Wolfgang Goethe University - ITP/JWGU, Frankfurtam Main, Germany

72. MARIA FLORENCIA IZZO VILLAFANE - Universidad Nacional de LaPlata, Buenos Aires, Argentina

73. MARIANA CHINAGLIA - Universidade Federal de Sao Carlos - UFSCar,Sao Carlos, Brazil

74. MARIO LUIZ LOPES DA SILVA - Universidade Federal de Pelotas -UFPEL, Pelotas, Brazil


75. MATHEUS BROILO - Universidade Federal do Rio Grande do Sul -UFRGS, Porto Alegre, Brazil

76. MAURO MARIANI - Facultad de Ciencias Astronomicas y Geofısicas,Universidad Nacional de La Plata - FCAG/UNLP, La Plata, Argentina

77. MIGUEL DE CAMPOS - Universidade Federal de Roraima - UFRR, BoaVista, Brazil

78. MOISES RAZEIRA - Universidade Federal do Pampa - UNIPAMPA,Cacapava do Sul, Brazil

79. MONICA TERGOLINA - Universidade Federal do Rio Grande do Sul -UFRGS, Porto Alegre, Brazil

80. NADJA SIMAO MAGALHAES - Universidade Federal de Sao Paulo -UNIFESP, Sao Paulo, Brazil

81. NILO SERPA - Faculdades Integradas Promove - ICESP, Brasılia, Brazil

82. NORBERTO SCOCCOLA - Comision Nacional de Energıa Atomica -CNEA, Buenos Aires, Argentina

83. OLIVIER PIGUET - Universidade Federal de Vicosa - UFV, Vicosa,Brazil

84. OMAIR ZUBAIRI - Department of Sciences, Wentworth Institute of Tech-nology - WIT, Boston, USA

85. ORLENYS NATALI TROCONIS - Universidade Federal Fluminense -UFF, Niteroi, Brazil

86. PAULO ROBERTO MURGER NOGUEIRA - Instituto Federal de Ed-ucacao, Ciencia e Tecnologia de Sao Paulo - IFSP, Sao Paulo, Brazil

87. PASCAL CHARDONNET - University of Savoie - US, Savoie, France

88. PEDRO CUNHA DE HOLANDA - Universidade Estadual de Campinas- UNICAMP, Campinas, Brazil

89. PEDRO DA CUNHA FERREIRA - Universidade Federal do Rio Grandedo Norte - UFRN, Natal, Brazil

90. PEDRO HENRIQUE GOULART CARDOSO - Universidade Federal deSanta Catarina - UFSC, Florianopolis, Brazil

91. PEDRO MORAES- Instituto Tecnologico de Aeronautica - ITA, Sao Josedos Campos, Brazil

92. PETER OTTO HESS - Instituto de Ciencias Nucleares, Universidad Na-cional Autonoma de Mexico - ICN/UNAM, Mexico

93. RAFAEL CAMARGO RODRIGUES DE LIMA - Universidade do Estadode Santa Catarina - UDESC, Florianopolis, Brazil


94. REINALDO ROBERTO ROSA - Laboratorio Associado de Computacaoe Matematica Aplicada - LAC, Instituto Nacional de Pesquisas Espaciais- INPE, Sao Jose dos Campos, Brazil

95. REMO RUFFINI - International Centre for Relativistic Astrophysics Net-work ICRANet, Pescara; Sapienza - Universita di Roma, Roma, Italy

96. RENAT ANASOVICH SULTANOV - St. Cloud State University, St,Cloud, USA

97. RICARDO L.S. FARIAS - Universidade Federal de Santa Maria - UFSM,Santa Maria, Brazil

98. RODOLFO VALENTIM - Instituto de Astronomia, Geofısica e CienciasAtmosfericas, Universidade de Sao Paulo - IAG/USP, Sao Paulo, Brazil

99. RODRIGO ALVARES DE SOUZA - Instituto de Astronomia, Geofısica eCiencias Atmosfericas, Universidade de Sao Paulo - IAG/USP, Sao Paulo,Brazil

100. RODRIGO FRANCISCO DOS SANTOS - Universidade Federal Flumi-nense - UFF, Niteroi, Brazil

101. RODRIGO NEMMEN - Universidade de Sao Paulo - USP, Sao Paulo,Brazil

102. RODRIGO PICANCO NEGREIROS - Universidade Federal Fluminense- UFF, Niteroi, Brazil

103. ROGERIO MENEZES DE ALMEIDA - Universidade Federal Fluminense- UFF, Niteroi, Brazil

104. RONALDO VIEIRA LOBATO - Instituto Tecnologico de Aeronautica -ITA, Sao Jose dos Campos, Brazil

105. ROSANA DE OLIVEIRA GOMES - Universidade Federal do Rio Grandedo Sul - UFRGS, Porto Alegre, Brazil

106. RUBENS DE MELO MARINHO JUNIOR - Instituto Tecnologico deAeronautica - ITA, Sao Jose dos Campos, Brazil

107. SAMUEL ISIDORO DOS SANTOS JUNIOR - Instituto Tecnologico deAeronautica - ITA, Sao Jose dos Campos, Brazil

108. SERGEY BURDIN - University of Liverpool, Liverpool, United Kingdom

109. SERGIO BARBOSA DUARTE - Centro Brasileiro de Pesquisas Fısicas -CBPF, Rio de Janeiro, Brazil

110. S.O. KEPLER - Universidade Federal do Rio Grande do Sul - UFRGS,Porto Alegre, Brazil

111. SONY MARTINS - Universidade Federal do Rio Grande do Sul - UFRGS,Porto Alegre, Brazil


112. STEFAN SCHRAMM - Frankfurt Institute for Advanced Studies - FIAS,Frankfurt am Main, Germany

113. THAISA STORCHI BERGMANN - Universidade Federal do Rio Grandedo Sul - UFRGS, Porto Alegre, Brazil

114. THIAGO VINICIUS MOREIRA GUIMARAES - Universidade EstadualPaulista - UNESP, Sao Paulo, Brazil

115. THOMAS BOLLER - Max-Planck-Institut fur Extraterrestrische Physik- MPE, Garching, Germany

116. VINCENZO LICCARDO - Instituto Tecnologico de Aeronautica - ITA,Sao Jose dos Campos, Brazil

117. VIVIANE ANGELICO PEREIRA ALFRADIQUE - Universidade FederalFluminense - UFF, Niteroi, Brazil

118. WEN ZHAO - University of Science and Technology of China - USTC,Hefei, China

quarks and cosmos book of abstracts - my web page

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