particle physics lesson from core...
TRANSCRIPT
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Workshop on Off-the-Beaten-Track Dark Matter and Astrophysical Probes of Fundamental Physics
ICTP, Trieste 13-17 April 2015
PARTICLE PHYSICS LESSON FROM CORE-COLLAPSE SUPERNOVAE
Alessandro MIRIZZIUniversity of BARI, Italy
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN1987A neutrinos
Particle physics lesson from SN1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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Core collapse SN corresponds to the terminal phase of a massive star [M ≳ 8 M
]which becomes unstable at the end of its life. It collapses and ejects its outermantle in a shock wave driven explosion.
SUPERNOVA NEUTRINOS
n
n
n
n
n
n
n
n
TIME SCALES: Neutrino emission lasts ~10 s
EXPECTED: 1-3 SN/century in ourgalaxy (d O (10) kpc).
ENERGY SCALES: 99% of thereleased energy (~ 1053 erg) isemitted by n and n of all flavors,with typical energies E ~ O(15 MeV).
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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Onion-like layers of a massive, evolved star just before core collapse.
CollapseNuclear density
Core-bounce & shock wave
shock-wave stalling Shock revival
LIFE AND DEATH OF A MASSIVE STAR
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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[Figure adapted from Fischer et al. (Basel group), arXiv: 0908.1871]10. 8 Msun progenitor mass
(spherically symmetric with Boltzmnann n transport)
Neutronization burst Accretion Cooling
• Shock breakout• De-leptonization of outer core layers
• Shock stalls ~ 150 km• n powered by infalling matter
• Cooling on n diffusion time scale
THREE PHASES OF NEUTRINO EMISSION
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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SN AS LABORATORY FOR NEUTRINO NSI
Examples of FCNC:
Rp violating SUSY
Minimal Flavor Violation Hypothesis
Lepto-Quark Models
Stellar environment is sensitive to neutrino flavor changing scatterings on heavy nuclei [see Amanik & Fuller, astro-ph/0606607, Lychkovskiy, Blinnikov, Vysotsky, 0912.1395]
Neutrino flavor changing neutral currents (FCNC)
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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QUALITATIVE EFFECT
,e n n
Open holes in neutrino sea, allow electron capture to proceed
ee p nn
Net reduction in Ye
After trapping and before bounce, levels of the FD seas of neutrinos:
Cross section for e- capture > cross section for FC scatteringso holes opened in the ne are immediately replaced by electron capture
ne level remains the same
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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Lower Ye
Lower initial shock energy
More outer core material for the shock to pass through
Disfavour getting explosion
Existence of n and nMore neutrinos partecipating indepositing energy behind the shock
Favour getting explosion
SN model is significantly changed!
LHC may see physics of this type- then it must be included in SN model
Alessandro Mirizzi ICTP Trieste, 16 April 2015
3/10
Yf
eiE
MYM ehc 8.52
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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Sanduleak 69 202
Large Magellanic Cloud
Distance 50 kpc
(160.000 light years)
Tarantula Nebula
Supernova 1987A
23 February 1987
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Neutrino Astronomy
Neutrino Burst Observation :
First verification of stellar evolution mechanism
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NEUTRINO SIGNAL OF SN 1987A IN KAMIOKANDE
SN 1987A
Background noise
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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Kamiokande-II (Japan)Water Cherenkov detector2140 tonsClock uncertainty 1 min
Irvine-Michigan-Brookhaven (US)Water Cherenkov detector6800 tonsClock uncertainty 50 ms
Baksan Scintillator Telescope(Soviet Union), 200 tonsRandom event cluster ~ 0.7/dayClock uncertainty +2/-54 s
NEUTRINO SIGNAL OF SUPERNOVA 1987A
Within clock uncertainties,signals are contemporaneous
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[e.g.,B. Jegerlehner, F. Neubig and G. Raffelt, PRD 54, 1194 (1996); A.M., and G. Raffelt, PRD 72,
063001 (2005)]
In agreement with the most recent theoretical predictions (i.e. Basel & Garching models)
Tota
l bin
din
g e
ne
rgy
Average ne energy
INTERPRETING SN 1987A NEUTRINOS
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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PARTICLE PHYSICS LESSON FROM SN 1987A
Exotic neutrino properties
Axion-like particles
Energy-loss and novel particles
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BOUND ON SECRET NEUTRINO INTERACTIONS
f new scalar mediator with mass M
Four fermion approximation2
2
1
4
gG
M
Requiring that n from cosmic sources travel through the CnB withoutscattering induced by the secret interactions leads to upper limits on thenew coupling.
8 2~ 10G GeV
SN1987A bound
Ng & Beacom, 1404.2288
[Kolb & Turner, PRD 36, 2895 (1987)]
Alessandro Mirizzi ICTP Trieste, 16 April 2015
nfngL
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Neutrinos severalhours before light
SN1987A BOUNDS ON NEUTRINO VELOCITY
[Evslin, 1111.0733 ]
SN1987A few events provide the moststringent constraints on n velocity. Crucialfor comparison with recent OPERA claim
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PARTICLE PHYSICS LESSON FROM SN 1987A
Exotic neutrino properties
Axion-like particles
Energy-loss and novel particles
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(ALPs)
Primakoff process: Photon-ALP transitions in external static E or B field
Photon-ALP conversions in macroscopic B-fields
AXION-LIKE PARTICLES (ALPs)
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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ALPs CONVERSIONS FOR SN 1987A
SN 1987AMilky-Way SMM Satellite
ALPs produced in SN core by Primakoff
process
ALP-photon conversions in the Galactic B-fields
No excess gamma-rays in coincidence
with SN 1987A
In [Payez, Evoli, Fischer, Giannotti, A.M. & Ringwald, 1410.3747] we revaluate the bound with
state-of-art models for SNe and Galactic B-fields
accurate microscopic description of the SN plasma
[Brockway, Carlson, Raffelt, astro-ph/9605197, Masso and Toldra, astro-ph/9606028]
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ALP-PHOTON FLUXES FOR SN 1987A
[Payez, Evoli, Fischer, Giannotti, A.M. & Ringwald, 1410.3747]
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GAMMA-RAY OBSERVATION FROM SMM SATELLITE
SN 1987A10s fluencelimits
0.4 cm2
0.6 cm2
0.9 cm2
Counts in the GRS instrument on the Solar Maximum Mission Satellite
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NEW BOUND ON ALPs FROM SN 1987A
[Payez, Evoli, Fischer, Giannotti, A.M. & Ringwald, 1410.3747]
SN1987A provides the strongest bound on ALP-photon coversions for ultralightALPs
for
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PARTICLE PHYSICS LESSON FROM SN 1987A
Exotic neutrino properties
Axion-like particles
Energy-loss and novel particles
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ENERGY-LOSS ARGUMENT
Volume emission of novel particles
Emission of very weaklyinteracting particles would“steal” energy from theneutrino burst and shorten it.
for r 3 1014 g cm-3 and T 30 MeV
Assuming that the SN 1987A neutrino burst was not shortened by more than ~½leads to an approximate requirement on a novel energy-loss rate of
ex < 1019 erg g1 s1
neutrino-sphere
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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AXION EMISSION FROM A NUCLEAR MEDIUM
NN NNa
nucleon-nucleon bremsstrahlung
5.3
3015
-1-1392s g erg102 TgaNa re
3-15
15
30
cm g10/
MeV 30/
rr
TT
4.1
4.0
5.3
30
15
T
r10
10
<aNg
Non-degenerate energy-loss rate
int 52 2
AN N
N N
a a
C CL a j a
f f
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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SN1987A AXION LIMITS
Free streaming[Burrows, Turner& Brinkmann,PRD 39:1020,1989]
Trapping[Burrows, Ressell& Turner, PRD 42:3297,1990]
Axion diffusionfrom an ‘’axion-sphere‘’
ExcludedVolume emission of axions
Possible detection in a water Cherenkov detector via oxygen nuclei excitation
Hadronic axion (ma ~ 1 eV, fa~106 GeV) not excluded by SN1987A. Possiblehot-dark matter candidate. The ‘’hadronic axion window’’ is closed bycosmological mass bounds.
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SN1987A BOUND ON HIDDEN PHOTONS
[Kazanas, Mohapatra et al., 1410.0221]
'L F F
n
ne mixing angle
U(1)’ gauge field of ‘
Energy-loss argument
Electromagnetic decays (‘ → e+ e-) [bounds of fluence of gamma-rays]
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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SN1987A BOUND ON KeV STERILE NEUTRINOS
[ Raffelt & Zhou, 1102.5124]
KeV sterile n are produced in a SN core by the mixing with active n.
For sufficiently small mixing q, ns
escape the core immediately after the production contributing to the energy-loss.
When both q and ms are sufficiently large ns are trapped in the SN core. However, since they have the largest free-path they contribute to the energy transfer, reducing once more the duration of the n signal.
Warm Dark Matter range is essentially unconstrained.
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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WHAT WE LEARNT FROM SN1987A?
General confirmation of core-collapse paradigm (total energy, spectra, timescale)
No unexpected energy-loss channel: Restrictive limits on axions, large extra-dimensions, right-handed neutrinos, etc…..
Improving Energy-Loss Limits with Next Supernova?
Even a relatively low-statistics new measurement could confirm generalvalidity of SN 1987A energy-loss limits
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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Large Detectors for Supernova Neutrinos
In brackets events for a “fiducial SN” at distance 10 kpc
HALO (tens) LVD (400)Borexino (80)
Super-Kamiokande(104)
KamLAND (330)
IceCube (106)
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NEXT-GENERATION DETECTORS
Mton scale water Cherenkov detectors
HYPER-KAMIOKANDE
MEMPHYS
GLACIER, LBNE
30-100 kton Liquid Argon TPC
20-50 kton scintillator
JUNO
LENA
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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SNAPSHOT OF SN DENSITIES
• Matter bkg potential
• nn interaction
n nGF2
~ R-3
~ R-2
eF NG2
E
m
2
2
• Vacuum oscillation frequencies
When >>, SN n oscillations dominated by n-n interactions
Equivalent n
density ~R2
[Tomas et al., astro-ph/0407132]
Collective flavor transitions at low-radii [O (102 – 103 km)]
Far more complicated than expected Spontaneous symmetry breaking in collective oscillations!
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SUPPRESSION OF COLLECTIVE OSCILLATIONS
At the moment, predictions are more robust in the phases where collectiveeffects are suppressed, i.e.:
Neutronization burst (t < 20 ms): large ne excess and nx deficit[Hannestad et al., astro-ph/0608695]
Accretion phase (t < 500 ms): dense matter term dominates over nu-nuinteraction term [Chakraborty, A.M. , Saviano et al., 1104.4031, 1105.1130, 1203.1484,
Sarikas et al., 1109.3601]
Large flux differences during the neutronization and accretion phase
Best cases for n oscillation effects !
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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Mixing parameters: U = U (q12, q13, q23, d as for CKM matrix
Mass-gap parameters: M2 = - , + , ± m2dm2
2dm2
2
“solar” “atmospheric”
normal hierarchy
inverted hierarchy
dm2/2
-dm2/2
m2
m2
dm2/2
-dm2/2
n1 n1n2 n2
n3
n3
3n FRAMEWORK
13 13 12 12 1
23 23 12 12 2
23 23 13 13 3
1
1
1
i
e
i
c e s c s
c s s c
s c e s c
d
d
n n
n n
n n
c12= cos q12, etc., d CP phase
SN neutrinos are sensitive to the unknown mass hierarchy
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NEUTRONIZATION BURST
ne,x e- ne,x e-
pb
0.4 Water Cherenkov
pb
100 kton LAr
Robust feature of SN simulations
[Kachelriess et al., astro-ph/0412082, Gil-Botella & Rubbia, hep-ph0307244]
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PROBING eV STERILE NU WITH NEUTRONIZATION BURST
[Esmaili, Peres & Serpico, 1402.1453]
3+1 scheme
IH: disappearence of neutronization peak. Possible appearence of delayed peak due to the fraction of heavy n4 component in ne (kinematical reason).
Peculiar time-energy distribution in LAr TPC.
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RISE TIME OF SN NEUTRINO SIGNAL IN ANTI-NU
The production of ne is more stronglysuppressed than that of nx during thefirst tens of ms after bounce because ofthe high degeneracy of e and ne .
ne are produced more gradually via ccprocesses (e captures on free nucleons)in the accreting matter; nx come fastlyfrom a deeper region
The lightcurves of the two species in thefirst O(100) ms are quite different.
ne
nx
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RISE TIME ANALYSIS: HIERARCHY DETERMINATION
SN n signal in IcecubeIn accretion phase one has
NH
IH
A high-statistics measurment of therise time shape may distinguish the twoscenarios
Are the rise time shapes enough robustlypredicted to be useful?
Models with state-of-the art treatment of weak physics (Garching simulations) suggest so: one could attribute a ‘’shape’’ to NH and IH.
[see Serpico, Chakraborty, Fischer, Hudepohl, Janka & A.M., 1111.4483]
Cumulative distribution
Given these promising early results, it wouldbe mandatory in future to explore therobusteness of the signature with othersimulations. [see Ott et al., 1212.4250]
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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DIFFUSE SUPERNOVA NEUTRINO BACKGROUND
Approx. 10 core collaspes/sec in the visible universe
Emitted n energy density~extra galactic bkg light
~ 10% of CMB density
Detectable ne flux at Earth~ 10 cm-2s-1
mostly from redshift z~1
Confirm the star formation rate
Nu emission from average core-collapse & black-hole formation
Pushing frontiers of neutrino astronomy to cosmic distances!
Windows of opportunity btw reactor ne and atmospheric n bkg
[Beacom & Vagins, hep-ph/0309300]
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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CONSTRAINT OF NU INVISIBLE DECAY FROM DSNB
'n n f
Nu decay in Majoron
DSNB can probe lifetimes of cosmological interest
01 /i
i
EH
m
DSNB spectrum larger, comparable or smaller than the standard one
[Fogli, Lisi, A.M., Montanino, hep-ph/0401227]
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OUTLINE
Introduction to SN neutrinos
SN neutrinos & NSI
SN 1987A neutrinos
Particle physics lesson from SN 1987A
SN neutrino oscillations
Conclusions
Alessandro Mirizzi ICTP Trieste, 16 April 2015
Diffuse SN neutrino background (DSNB)
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CONCLUSIONS
Observing SN neutrinos is the next frontiers of low-energy neutrinoastronomy
The physics potential of current and next-generation detectors inthis context is enormous, both for particle physics andastrophysics.
Neutrino signal duration provides most useful particle-physicsinformation. Neutrino signal from next nearby SN would make thisargument much more precise.
Flavor conversions in SNe would provide valuable information on theneutrino mass hierarchy. Further investigations necessary oncollective oscillations.
Alessandro Mirizzi ICTP Trieste, 16 April 2015
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THANK YOU!