SOLARNET 5 School & Workshop Waves and Oscillations in the Solar Atmosphere

Queen’s University Belfast, 25th August - 2nd September 2016

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SOLARNET 5 School & Workshop 1Waves and Oscillations in the Solar Atmosphere 1

School Information 3

School Schedule 4

Workshop Schedule 5

Workshop Talks 6

Workshop Abstracts 8

School & Workshop Venues 25

Social Events 25

Tourist Information 25

Queen’s Campus Map 26

Directions from Elms Village to School 27

Directions from Queen’s to Cutters Wharf 28

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School Information

Invited School Speakers

• Inigo Arregui, Instituto de Astrofísica de Canarias (IAC), Spain• Ineke De Moortel, The University of St. Andrews, UK• Robertus Erdélyi, The University of Sheffield, UK• Laurent Gizon, Max-Planck-Institut für Sonnensystemforschung (MPS), Germany• Marcel Goossens, Katholieke Universiteit (KU) Leuven, Belgium• David Jess, Queen's University Belfast, UK• Peter Keys, Queen's University Belfast, UK• James McLaughlin, Northumbria University, UK• Stuart Mumford, The University of Sheffield, UK• Hector Socas Navarro, Instituto de Astrofísica de Canarias (IAC), Spain• Oskar Steiner, Kiepenheuer-Institut für Sonnenphysik (KIS), Germany• Tom Van Doorsselaere, Katholieke Universiteit (KU) Leuven, Belgium• Sven Wedemeyer, Universitetet i Oslo (UiO), Norway• Penny Wu, The University of Delaware, USA• Teimuraz Zaqarashvili, Institut für Weltraumforschung, Austria

Lecture Topics

• Prominence Seismology (Arregui)• Waves and Flows in the Solar Corona (De Moortel)• Wave Modes in the Solar Atmosphere (Erdélyi)• Helioseismology and the Solar Interior (Gizon)• Waves in the Solar Atmosphere: Properties and History (Goossens)• Techniques for Retrieving Wave Properties from Observations (Jess)• Ground-based Observatories and Image Reduction Techniques (Keys)• Oscillatory Reconnection (McLaughlin)• Python and SunPy for Solar Physicists (Mumford)• Spectropolarimetric Stokes Inversions (Socas Navarro)• MHD Simulations (Steiner)• Multi-stranded Flux Tubes and their effects on Wave Propagation (van Doorsselaere)• Solar Science with ALMA and other Radio Telescopes (Wedemeyer)• Turbulence (Wu)• Rossby Waves (Zaqarashvili)

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School ScheduleDay\Time

Thursday 25th

Friday 26th

Saturday 27th

Sunday 28th

Monday 29th

Tuesday 30th

09:00 - 10:30

Marcel Goossens

Sven Wedemeyer

Free Weekend Peter Keys Inigo Arregui

10:30 - 11:00

Coffee Coffee Coffee Coffee

11:00 - 12:30

Penny Wu Oskar Steiner

David Jess Laurent Gizon

12:30 - 13:30

Lunch Lunch Lunch Lunch

13:30 - 15:00

James McLaughlin

Stuart Mumford

Tom van Doorsselaere

Robertus Erdelyi

15:00 - 15:30

Coffee Coffee Coffee Coffee

15:30 - 17:00

Hector Socas

Navarro

Stuart Mumford

Teimuraz Zaqarashvili

Ineke De Moortel

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Workshop Schedule

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Wednesday 31st Thursday 1st

09:00 - 10:30 Russell, Philishvili,

Korsos, Prochazka

Pascoe, Pagano,

Van Doorsselaere, Karampelas

10:30 - 11:00 Coffee Coffee

11:00 - 12:40 Bello Gonzalez, Chagiashvili, DumbadzeMooroogen

Banerjee, Kanella, Howson,Prasad

12:40 - 14:00 Lunch Lunch

14:00 - 15:30 Utz, Gurgenashvili,

Reid,Barbulescu

Cauzzi, Ali Elden, Henriques,

KuridzeLosada

15:30 - 16:00 Coffee Coffee

16:00 - 17:40 Leenarts, Sandor Kiss,

Nelson,Vashalomidze

Morton,Gilbert,

Wu,Kourakis

Workshop TalksInvited Talks:

• MHD waves in coronal holes - Dipankar Banerjee

• Waves phenomena in Sunspots - Nazaret Bello Gonzalez

• Heating & Dynamics in the Quiet Chromosphere: The Role of Acoustic Shocks - Gianna Cauzzi

• Chromospheric diagnostics - Jorrit Leenarts

• Alfvenic waves in the corona - Richard Morton

• Coronal seismology using damped kink oscillations - David Pascoe

• The generation, propagation, and dissipation of slow magnetoacoustic waves in sunspots - Krishna Prasad

• Alfvén wave heating in solar flares - Alex Russell

• Magnetic bright points seen from observations, simulations and as possible wave guides - Dominik Utz

• Some recent insights into solar wind turbulent dissipation and heating - Penny Wu

Contributed Talks:

• Studying the characteristics of shock wave associated with CME using solar radio bursts - Khaled Ali Elden

• The Effect of Flows on the Propagation of MHD Waves Along a Magnetic Slab in an Asymmetric Environment - Mihai Barbulescu

• Flare-Related Brightenings in the active region NOAA 11429 - Tamar Chagiashvili

• On the long-period oscillations of the active region patterns: Method of least-square mapping on second order curves - Gulsun Dumbadze

• Quantifying Line-of-Sight Effects for Spectroscopic Measurements of Alfven Waves and Turbulence in the Solar Corona - Chris Gilbert

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• Rieger-Type Periodicity During Solar Cycles 14-24: Estimation of Dynamo Magnetic Field Strength in the Solar Interior - Eka Gurgenashvili

• A proven chromosphere to corona connection via jets in the quiet Sun - Vasco Henriques

• The Effects of Heat Transfer on a Coronal Model with a Photospheric Driver - Thomas Howson

• Investigating 4D (3D + Time) Solar Coronal (Joule) Heating Events In MHD Simulations - Charalambos Kanella

• Heating by propagating transverse waves in simulated coronal loops - Konstantinos Karampelas

• 3D investigation of flaring solar Active Regions - Marianna Korsos

• Nonlinear waves in non-Maxwellian Space plasmas - Ioannis Kourakis

• Kelvin-Helmholtz instability in solar chromospheric jets - David Kuridze

• Formation of sunspots: theory and observations - Illa R Losada

• Measuring kink waves in the internetwork H-alpha chromosphere - Krishna Mooroogen

• The Relationship Between Cancellation and UV Bursts – Chris Nelson

• Contribution of coupling of Alfvén and kink modes to coronal heating - Paolo Pagano

• Pre-flare quasi-oscillatory dynamics observed in flaring loop system on March 6, 2012 - Elena Philishvili

• Suppression of Hydrogen Emission in an X-class White-light Solar Flare – Ondrej Prochazka

• Photospheric Inversions of Ellerman Bombs - Aaron Reid

• New temporal properties of chromospheric macrospicules - Tamas Sandor Kiss

• Forward modelling of coronal oscillations for seismology - Tom Van Doorsselaere

• Formation and evolution of coronal rain observed by SDO/AIA on February 22, 2012 - Zurab Vashalomidze

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Workshop Abstracts

Wednesday 31st of August

Morning Session 1 (09:00 - 10:30)

Alex Russell, University of Dundee [09:00 - 09:30]

Alfvén wave heating in solar flares

It might seem obvious that waves and Poynting flux could be important in solar flares – flares are highly dynamic, they transport large amounts of energy from the corona to the chromosphere, and Poynting flux is often the dominant energy transport in solar plasmas (e.g. its importance in coronal heating discussions). However, for various reasons the flare community has only recently begun to concertedly investigate whether flare models are improved by including waves alongside energetic particles and thermal conduction. This talk gives an overview of a young and exciting research area, focusing on a few recent important results. In it, I will argue that MHD waves are an intrinsic part of magnetic reconnection in the impulsive phase of flares, that downgoing MHD waves are capable of heating the lower atmosphere and driving explosive evaporations, and that a three-dimensional dynamic understanding of flares – incorporating waves – helps to resolve longstanding challenges as well as new ones presented by the latest observations.————————————————————————————————————

Elena Philishvili, Ilia State University [09:30 - 09:50]

Pre-flare quasi-oscillatory dynamics observed in flaring loop system on March 6, 2012

E. Philishvili, B.M. Shergelashvili, T.V. Zaqarashvili, V. Kukhianidze, G.Ramishvili , M. Khodachenko, S. Poedts, P. De CausmaeckerIlia State University,  KU Leuven

We studied dynamics of the flaring loops in active region (AR) 11429. The observed dynamics consists of several stages of the flaring loop system evolution in time during ascending and descending phases of the registered M class flare. These dynamical properties also can be classified by different types comprising of reconnection related plasma ejection and aperiodic flows, quasi-periodic oscillatory motions, rapid temperature and density changes etc. Our goal was investigation of the spatial and temporal behavior of the magnetic loop structures during the ascending (pre-flare) phase, within which the loop system clearly showed quasi-periodic behavior both in space and time. We have studied characteristic location of the detected bright blobs along the coronal loop, motion and periodicity properties by examining space-time diagrams and intensity variation analysis using AIA intensity and HMI magnetogram images from the Solar Dynamics Observatory (SDO) instruments. We have obtained periods of oscillations.

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We present two different interpretations for the observed dynamics. Firstly, the oscillations can be the manifestation of non-fundamental harmonics of longitudinal standing acoustic oscillations driven by the thermodynamically nonequilibrium background with variable in time density and temperature. The Second possible interpretation we give is that the observed bright blobs could be a signature of strongly twisted coronal loop unstable w.r.t. kink instability.————————————————————————————————————

Marianna Korsos, The University of Sheffield [09:50 - 10:10]

3D investigation of flaring solar Active Regions

Here, we present new studies of the pre-flare behaviour and evolution of Active Regions (ARs). We employ SOHO/MDI and SDO/HMI data, introduce and apply the so-called weighted horizontal gradient of magnetic field (WG_M), defined between opposite polarity spot-groups closer to the polarity inversion line of ARs. This WG_M parameter has the potential to yield important diagnostic information (i) about a more accurate prediction of onset time and (ii) on predicting flare intensity (currently) from C to X class flares.

Next, we will demonstrate how by tracking the temporal evolution of W_GM, the distance between opposite polarity spots and the associated net flux at various heights in the lower solar atmosphere can considerably improve flare forecasting. We demonstrate that the temporal behaviour of WG_M across the chromosphere-low corona interface has new forecast capabilities. We found, that at a certain height within this interface region the converging of opposite polarities begins much earlier than at the photosphere or at other atmospheric heights. We found that the gained forecast capability time could be as high as about 10-12 hrs. Therefore our tool, by identifying the optimum height in the solar atmosphere for flare forecasting, may considerably increase Space Weather predictability.————————————————————————————————————

Ondrej Prochazka, Queen’s University Belfast [10:10 - 10:30]

Suppression of Hydrogen Emission in an X-class White-light Solar Flare

We present an analysis of an X-class flare that occurred on 11 June 2014 in active region NOAA 12087 using a newly developed high cadence Image Selector operated by Astronomical Institute in Ondrejov, Czech Republic. This instrument provides spectra in the 350-440 nm wavelength range, which covers the higher order Balmer lines as well as the Balmer jump at 364 nm. However, no detectable increase in these emissions were detected during the flare, and support observations from SDO/EVE MEGS-B show that the Lyman line series and recombination continuum were also suppressed, particularly when compared to two other X-class flares on the preceding day. The X-class flare under investigation also showed strong white light emission in SDO/HMI data, as well as an extremely hard electron spectrum (delta~3.6), and gamma-ray emission, from RHESSI data. This unique combination of datasets allows us to conclude that the white light emission from this flare is more consistent with blackbody radiation than chromospheric hydrogen emission. In contrast to what is predicted from standard thick target

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model, radiative hydrodynamic modelling shows that the observed spectra can be reproduced by directly heating the temperature minimum region in the photosphere, rather than the chromosphere.————————————————————————————————————

Morning Session 2 (11:00 - 12:30)

Nazaret Bello Gonzalez, KIS Freiburg [11:00 - 11:30]

Wave phenomena in Sunspots

The highly dynamic magnetised solar atmosphere exhibits a wealth of oscillatory magnetohydrodynamic (MHD) modes. In this talk, the oscillatory phenomena present in sunspots from an observational point of view will be reviewed.————————————————————————————————————

Tamar Chagiashvili, Ilia State, Georgia [11:30 - 11:50]

Flare-Related Brightenings in the active region NOAA 11429

Solar magnetic field interaction with plasma controls the most dynamical processes and topological changes in various coronal structures. Even small variations in dense photospheric plasma and/or magnetic field may lead to the most catastrophic eruptions, such as solar flares and CMEs. Moreover, plasma and magnetic field interaction has its important effect on the photosphere itself. The good example of it is the White light flare. White light flares are rare phenomena. They were believed to occur only with high energy flares. But recent high-resolution detectors revealed that they are characteristic for all flares. It is crucial to study WLFs to understand the physical and morphological changes of the solar photosphere.

The subject of our research is to study WLFs after high- energy X- and M –class flares. We are particularly interested in the behavior of the photospheric changes and its characteristics. For this reason, we studied the evolution of the well-developed sunspot of NOAA Active Region 11429. The active region hosted two X 5.4 and X 1.3 flares on March 7, 2012. They occurred in one hour interval with starting times 00:02 and 01:05 respectively. The first flare lasted 40 minutes and the second - 17 minutes. We studied flare related white light emission, calculated their movement, measured energies and built the model which may explain the movement of the emission. This field is not new as WLFs has been studied for a long time, but because of the complexity of the photosphere, their features are not well understood yet.

Visual and methodological (running difference image, time slicing method) investigation of the observational data of HMI/SDO satellite revealed, that during the flares, because of the strong back-warming effect, white-light emissions emerge

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in the HMI continuum and crosses the sunspot (in the HMI magnetogram they are seen as the magnetic polarity change - in the black part the white pattern and in the white part, the black pattern). During the first flare, the brightening cropped up after the 11 minute of the flares start-time (recorded by GOES), traversed the sunspot and disappeared before the flare ended. In second case, the brightening began after a minute of flare starting time, continued 11-13 minutes and ended 6 minutes before the flare-end.

The patterns seen in the white – light continuum were co-spatial and co-temporal with the flare ribbons (in all EUV wavelengths of AIA). ————————————————————————————————————

Gulsun Dumbadze, Ilia State University [11:50 - 12:10]

On the long-period oscillations of the active region patterns: Method of least-square mapping on second order curves

G. Dumbadze, B.M. Shergelashvili, V. Kukhianidze, G. Ramishvili, T.V. Zaqarashvili, M. Khodachenko, E. Gurgenashvili, S. Poedts and P. De Causmaecker 

Active Regions (ARs) are major sources of a variety of solar dynamic events. The development of automated detection and identification tools for solar features is required for a deeper understanding of the solar cycle. We studied the oscillatory dynamics of two ARs: NOAA 11327 and NOAA 11726, using two different methods of pattern recognition. In this work we developed a novel method of automated AR border detection and used another existing method for the proof-of-the-concept. The first method is using least square fitting on the smallest ellipse enclosing the AR and the second method applies regression on the convex hull. After processing the data we found that the axes and the inclination angle of both the ellipse and the convex hull oscillate in time. These oscillations are interpreted as the second harmonic of the standing long-period kink oscillations (with the node at the apex) of the magnetic flux tube connecting the two main sunspots of the ARs. We also found that the inclination angles oscillate with the characteristic periods 4.9 hours in AR 11726 and 4.6 hours in AR 11327, respectively. In addition, we discovered that the lengths of the pattern axes in the ARs oscillate with similar characteristic periods and these oscillations are ascribed to standing global flute modes. In both ARs we have estimated the distribution of the phase speed magnitude along the magnetic tubes (along the two main spots) by interpreting the obtained oscillation of the inclination angle as the standing second harmonic kink mode. After comparison of the obtained results for fast and slow kink modes, we concluded that both of these modes are good candidates to explain the observed oscillations of the AR inclination angles (as in the high plasma β regime the phase speeds of these modes are comparable and of the order of the Alfvén speed). Based on the properties of the observed oscillations, we detected the appropriate depth of the sunspot patterns, which are in good agreement with existing helioseismic estimations of this depth. The latter analysis can be used as a base for the development of a magneto-seismological tool for ARs.

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Krishna Mooroogen, Northumbria University [12:10 - 12:30]

Measuring kink waves in the internetwork H- chromosphere

Current observational instruments are now providing data with the necessary temporal and spatial cadences required to examine highly dynamic, fine-scale magnetic structures in the solar atmosphere. Using a combination of monochromatic imaging and spectroscopy from the Swedish Solar Telescope, we investigate fibrils in the H- internetwork. Transverse oscillations are observed, which we interpret as the kink wave. The wave properties of the kink waves are measured and the properties are used, via inversion, to perform magneto-seismology. With this, we aim to provide statistics on the variation of plasma properties of the wave-guides.

We model the noise in the data to improve the uncertainties of the measurement of spatial and temporal properties of the waves. Using an advanced tracking and fitting routine we measure the periods and amplitudes of the waves along a wave-guide. Cross-correlation is utilised to measure the propagation speed of the waves. It is found that the seismological profiles of density, radius and magnetic field can be described solely by the amplitudes of the waves, a direct result from the measurement of constant propagation speeds. We find that whilst some of the profiles fit within the hydrostatic regime, most of the profiles do not, making them difficult to interpret. ————————————————————————————————————

Afternoon Session 1 (14:00 - 15:30)

Dominik Utz, KU Leuven and IAA Granada [14:00 - 14:30]

Magnetic Bright Points as seen from observations, simulations and as possible wave guides

D. Utz, T. Van Doorsselaere, O. Kuhner & N. Magyar

The Sun features a highly dynamic solar atmosphere which is hosting energetic events like flares and coronal mass ejections. All these dynamic phenomena are caused in the one or other way by magnetic fields and their dynamics. These magnetic fields are connected from the higher atmosphere via the chromosphere and photosphere to the solar interior.

Within the photosphere large and extended magnetic field build-ups are visible as sunspots and active regions. On the other hand, smaller, but not necessarily much weaker, magnetic fields form structures such as Magnetic Bright Points (MBPs).

MBPs are small-scale magnetic field concentrations (on the order of 100 km in diameter; 1 kG in magnetic field strength) seen on the surface of the Sun. They can be detected in the photosphere as bright pointlike features within intergranular lanes. As they represent, at least in a first approximation, isolated magnetic flux

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tubes, they are important candidates for MHD wave guides and thus able to connect energetically the lower solar atmosphere with the mid and possible higher atmosphere. Due to this fact, they likely play an important role for the heating of the upper atmosphere as well as for its mass balance.

In the current contribution we would like to give an introduction in the theory of MBPs as well as observations and simulations of their behaviour. Later on we will have a look on a few selected publications regarding waves in MBPs and small-scale magnetic field concentrations before we will finally present some own recent results as well as current work in progress.————————————————————————————————————

Eka Gurgenashvili, Ilia State, Georgia [14:30 - 14:50]

Rieger-Type Periodicity During Solar Cycles 14-24: Estimation of Dynamo Magnetic Field Strength in the Solar Interior

Solar activity undergoes a variation over timescales of several months known as Rieger-type periodicity, which usually occurs near maxima of sunspot cycles. An early analysis showed that the periodicity appears only in some cycles and is absent in other cycles. But the appearance/absence during different cycles has not been explained. We performed a wavelet analysis of sunspot data from the Greenwich Royal Observatory and the Royal Observatory of Belgium during cycles 14–24. We found that the Rieger-type periods occur in all cycles, but they are cycle dependent: shorter periods occur during stronger cycles. Our analysis revealed a periodicity of 185–195 days during the weak cycles 14–15 and 24 and a periodicity of 155–165 days during the stronger cycles 16–23. We derived the dispersion relation of the spherical harmonics of the magnetic Rossby waves in the presence of differential rotation and a toroidal magnetic field in the dynamo layer near the base of the convection zone. This showed that the harmonics of fast Rossby waves with m = 1 and n = 4, where m (n) indicates the toroidal (poloidal) wavenumbers, perfectly fit with the observed periodicity. The variation of the toroidal field strength from weaker to stronger cycles may lead to the different periods found in those cycles, which explains the observed enigmatic feature of the Rieger-type periodicity. Finally, we used the observed periodicity to estimate the dynamo field strength during cycles 14–24. Our estimations suggest a field strength of ∼40 kG for the stronger cycles and ∼20 kG for the weaker cycles.————————————————————————————————————

Aaron Reid, Queen’s University Belfast [14:50 - 15:10]

Photospheric Inversions of Ellerman Bombs

Ellerman Bombs are small-scale brightenings in the upper solar photosphere. Recent studies indicate the cause of these impulsive brightenings could be due to magnetic reconnection. We use high resolution Hα imaging spectroscopy along with Fe I 6302.5 Å spectro- polarimetry from the Swedish 1-m Solar Telescope (SST), combined with data from the Solar Dynamic Observatory (SDO) to study EBs and the evolution of the local magnetic fields at EB locations. The EBs are

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found via an EB detection and tracking algorithm. We find, using NICOLE inversions of the spectro-polarimetric data, that on average (3.43 ± 0.49) x 1024 ergs of stored magnetic energy disappears from the bipolar region during the EBs burning, of which 31.2% appears to transform into the radiative energy seen in the Hα observations. The inversions also show flux cancellation rates of 1014 - 1015 Mx s−1, and temperature enhancements of 500K.

————————————————————————————————————Mihai Barbulescu, the University of Sheffield [15:10 - 15:30]

The Effect of Flows on the Propagation of MHD Waves Along a Magnetic Slab in an Asymmetric Environment

We investigate linear MHD wave propagation along a magnetic slab in an asymmetric environment. We define the equilibrium as an infinite magnetic slab embedded in a plasma with different values of pressure, density, background uniform flow, and magnetic field on either side. We derive the dispersion relation for this system and discuss the effect of asymmetry of the equilibrium on the wave propagation along the slab. In this configuration, the classical symmetric and anti-symmetric modes of propagation in a slab - sausage and kink - appear to break down. Expressions describing the critical points where forward propagating waves become backward propagating due to the bulk flow motion, and for the Kelvin-Helmholtz instability are also presented. Applications to solar photospheric and upper atmospheric waveguides are presented.————————————————————————————————————

Afternoon Session 2 (16:00 - 17:30)

Jorrit Leenarts, Stockholm University [16:00 - 16:30]

Chromospheric diagnostics

Understanding the solar chromosphere requires understanding observations of the chromosphere. Chromospheric diagnostics are unfortunately difficult to interpret, because they typically form under non-LTE and sometimes non-ionization-equilibrium conditions. In this talk I will review the diagnostic value of the Mg II h&k lines observed with IRIS, the mm-continua observed with ALMA, and the Halpha and He I 1083 nm lines that are observed with various ground-based observatories.————————————————————————————————————

Tamas Sandor Kiss, University of Sheffield [16:30 - 16:50]

New temporal properties of chromospheric macrospicules

Macrospicules (MSs) are medium-scale jet-like phenomena in the chromosphere, which have a potential to transport momentum and energy from the lower solar atmospheric regions to the Transition Region and the corona. A detailed statistical analysis is conducted about their temporal and spatial behaviour for a better understanding of their physical properties. Based on the excellent spatial and temporal resolution observations provided by the Atmospheric Imaging Assembly

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(AIA) of Solar Dynamics Observatory (SDO), we constructed a 4.5-year long dataset, containing 258 macrospicules between June 2010 and December 2014 detected at 30.4 nm wavelength. Analysis of this dataset demonstrates many new attributes of MS: two-year-long oscillation in the maximum length (and other physical features) with a possible connection to the F10.7cm radio flux, asymmetry between the hemispheres in spatial distribution or their trajectories, and a link to the dynamo wave. ————————————————————————————————————

Chris Nelson, The University of Sheffield & Queen’s University Belfast [16:50 - 17:10]

The Relationship Between Cancellation and UV bursts

Cancellation observed in photospheric magnetograms is a potential indicator of energetic processes in the lower solar atmosphere. In this talk, we present an analysis of a range of cancellation features co-spatial to a variety of UV burst events, including IRIS bombs.  The key fundamental properties measured for these events include their cancellation rates, which could provide some information about the amount of energy available for deposition in the surrounding atmosphere. Comparisons between the temporal evolution of the local magnetic field and light curves constructed from a variety of co-spatial SDO/AIA wavelengths displays a potential relationship between short-lived increases in the cancellation rate and UV burst activity, potentially explaining how hour-long cancellation processes can correspond to UV busts with lifetimes of around 10 minutes. Overall, our results suggest that cancellation measured in the photosphere can account for the energy budgets of a range of UV bursts, however, it is by no means a guaranteeing condition for burst formation.————————————————————————————————————

Zurab Vashalomidze, Ilia State, Georgia [17:10 - 17:30]

Formation and evolution of coronal rain observed by SDO/AIA on February 22, 2012

Context. The formation and dynamics of coronal rain are currently not fully understood. Coronal rain is the fall of cool and dense blobs formed by thermal instability in the solar corona towards the solar surface with acceleration smaller than gravitational free fall.

Aims: We aim to study the observational evidence of the formation of coronal rain and to trace the detailed dynamics of individual blobs. Methods: We used time series of the 171 Å and 304 Å spectral lines obtained by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO) above active region AR 11420 on February 22, 2012.

Results: Observations show that a coronal loop disappeared in the 171 Å channel and appeared in the 304 Å line more than one hour later, which indicates a rapid cooling of the coronal loop from 1 MK to 0.05 MK. An energy estimation shows that

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the radiation is higher than the heat input, which indicates so-called catastrophic cooling. The cooling was accompanied by the formation of coronal rain in the form of falling cold plasma. We studied two different sequences of falling blobs. The first sequence includes three different blobs. The mean velocities of the blobs were estimated to be 50 km s-1, 60 km s-1 and 40 km s-1. A polynomial fit shows the different values of the acceleration for different blobs, which are lower than free-fall in the solar corona. The first and second blob move along the same path, but with and without acceleration, respectively. We performed simple numerical simulations for two consecutive blobs, which show that the second blob moves in a medium that is modified by the passage of the first blob. Therefore, the second blob has a relatively high speed and no acceleration, as is shown by observations. The second sequence includes two different blobs with mean velocities of 100 km s-1 and 90 km s-1, respectively.

Conclusions: The formation of coronal rain blobs is connected with the process of catastrophic cooling. The different acceleration of different coronal rain blobs might be due to the different values in the density ratio of blob to corona. All blobs leave trails, which might be a result of continuous cooling in their tails.————————————————————————————————————

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Thursday 1st of September

Morning Session 1 (09:00 - 10:30)

David Pascoe, The University of Warwick [09:00 - 09:30]

Coronal seismology using damped kink oscillations

Kink oscillations of solar coronal loops are frequently observed to be strongly damped. The damping can be explained by mode coupling so long as loops have a finite inhomogeneous layer between the higher density core and lower density background. The damping rate depends on the loop density contrast ratio and inhomogeneous layer width. The theoretical description for mode coupling has recently been extended to include the initial Gaussian damping regime in addition to the exponentially damped asymptotic state. Measuring the Gaussian and exponential damping times allows us to perform seismological inversions for the loop density profile. This seismological method allows the internal and external Alfven speeds to be calculated and used for improved estimates of the magnetic field strength or the phase mixing rate which is important for heating.————————————————————————————————————

Paolo Pagano, The University of St Andrews [09:30 - 09:50]

Contribution of coupling of Alfvén and kink modes to coronal heating

Recent observations of coronal loops reveal ubiquitous transverse velocity perturbations, that undergo strong damping as they propagate. Observational estimates show that these perturbations contain significant amounts of energy. We have previously demonstrated that this observed rapid damping can be understood in terms of coupling of different wave modes in the inhomogeneous boundaries of the loops: this mode coupling leads to the coupling of the transversal (kink) mode to the azimuthal (Alfvén) mode, observed as the decay of the transverse kink oscillations. However, an important point to note here is that (observed) wave damping does not automatically imply dissipation, and hence heating. To investigate under which circumstances this process can contribute to the coronal heating and to what extend the heating rate is sustainable, we perform 3D numerical experiments modelling the observed, transverse oscillations including the effects of resistivity, thermal conduction and radiative losses. We take into considerations different amplitudes of the driver, in a range from 2 km/s to 100 km/s, and model both single-harmonic and broadband drivers. Forward modelling is used to derive observable signatures.————————————————————————————————————

Tom Van Doorsselaere, KU Leuven [09:50 - 10:10]

Forward modelling of coronal oscillations for seismology

Tom Van Doorsselaere, Ding Yuan, Norbert Magyar, Sudip Mandal,Dipankar Banerjee

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The corona is optically thin and thus it is hard to interpret the observed intensity. This difficulty makes the study of coronal waves and seismology of them very hard, because it is not easy to connect the observed properties to theoretical models. In this presentation, I will introduce the Leuven forward modelling code FoMo. I will show recent results on the forward modelling of transverse waves and slow waves, and how the forward modelling can be used to improve the mode identification and seismology.————————————————————————————————————

Konstantinos Karampelas, KU Leuven [10:10 - 10:30]

Heating by propagating transverse waves in simulated coronal loops

Coronal loops are well studied prominent magnetic structures in the solar atmosphere, that stretch from the lower chromosphere up to the solar corona. Due to their physical characteristics, they are able to act as waveguides, transferring energy from the lower to the upper solar atmosphere, essentially connecting those different layers. In recent years, 3D magnetohydrodynamical simulations of flux tubes have established the significance of resonant absorption in the damping of standing transverse oscillations. The nonlinear nature of the mechanism has been examined alongside the Kelvin – Helmholtz instability, which is expected to manifest in the resonant layers. While it has long been hypothesized that these two mechanisms can also efficiently heat coronal loops, a severe shortcoming is that the heating only happens at the resonant location. This is expected to be found near the outer regions of the loops, where mixing with the hotter surroundings can easily hide this effect. In our project, we numerically simulate the effects of propagating transverse waves on both gravitationally stratified and non-stratified, straight, flux tubes, using continuous foot-point drivers of various amplitudes and frequencies. Our results show that large parts of our loops become turbulent as the resonant layer widens over time, efficiently spreading the wave heating over the entire loop cross-section. Different setups are used to distinguish between real heating due to turbulence and apparent heating due to the mixing of plasma of different temperatures. Alongside that, we show the effects of footpoint driving on the dynamics of the loop and the significance of the imposed oscillation frequency. Finally, we study the corresponding observable effects in the temporal and spatial evolution of the resonant layers in our flux tubes, by performing forward modelling.————————————————————————————————————

Morning Session 2 (11:00 - 12:40)

Dipankar Banerjee, IIA Bangalore [11:00 - 11:30]

MHD waves in coronal holes

Coronal holes are the dark patches in the solar corona associated with relatively cool, less dense plasma and unipolar fields. The fast component of the solar wind emanates from these regions. Several observations reveal the presence of magnetohydrodynamic (MHD) waves in coronal holes which are believed to play a key role in the acceleration of fast solar wind. The recent advent of high-resolution

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instruments had brought us many new insights on the properties of MHD waves in coronal holes. The advances made in the identification of compressive slow MHD waves in coronal holes, their possible connection with the recently discovered high- speed quasi-periodic up flows will be addressed. ————————————————————————————————————

Charalambos Kanella, UiO Norway [11:30 - 11:50]

Investigating 4D (3D + Time) Solar Coronal (Joule) Heating Events InMHD Simulations

C. Kanellas & B.V. Gudiksen

The “Solar Coronal Heating” problem is an unanswered question since 1939. It is unknown how the corona is heated up to more than 1 MK, while the photosphere has a temperature of roughly 6000 K. The answer to that is connected to the magnetic field, which transfer mechanical energy from the motions in the photosphere to the corona, store it and then release it. The magnetic field initially is in a force-free state and any excess energy is stored in the magnetic field in the form of current sheets, which are manifestation of distorted magnetic field. When current sheets are thin enough, magnetic reconnection can be triggered and generate flares and thus, a part of the stored energy is released and relaxing the system (Parker 1983a,b). In this model, many observationally unresolved flares occur at the same time and if the frequency is high enough, then this model could be a large contributor. The problem with the quantification of flares is that small events or many events cannot be resolved temporally or spatially due to the limitation of the current instrumentation and the background and foreground noise. Using MHD simulations (Bifrost code) we can simulate the Sun from the convection zone up to the corona. Performing a multiple threshold technique we are able to identify structures of any extend, shape and energy release in the joule heating term in Bifrost and resolve them temporally. Duration, energy release and integrated volume follow a power-law as a function of frequency of occurrence of each size, as expected from Self-Organized-Critical (SOC) systems. We find that nanoflares alone probably cannot heat the corona, flares can actually be a combination of many smaller events, the energy release from joule heating in each event does not happen at constant rate and strong correlations between energy, duration and integrated volume are found.————————————————————————————————————

Thomas Howson, The University of St Andrews [11:50 - 12:10]

The Effects of Heat Transfer on a Coronal Model with a Photospheric Driver

The convective driving of the photosphere can generate a Poynting Flux into the solar atmosphere that is sufficient to power coronal heating. A driver that is slow in comparison to the local Alfvén speed will build stresses in the atmospheric magnetic field, which can be released during reconnection events. Using the numerical code Lare3D, we present a coronal model that considers the effects of continuous driving on two magnetic flux-tubes. These initially straight tubes are allowed to relax towards a numerical equilibrium before a velocity field is imposed

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at the loop foot points. This rotational driver braids the flux-tubes around each other, forming intricate current sheets and inducing intense but highly localised heating. We include thermal conduction to determine how heat is re-distributed and consider its effects on both the plasma and the magnetic field. Further we investigate the magnitude of radiative cooling on the heating timescale in order to help establish the efficacy of the proposed heating mechanism.————————————————————————————————————

Krishna Prasad, Queen’s University Belfast [12:10 - 12:40]

The generation, propagation, and dissipation of slow magnetoacoustic waves in sunspots

Oscillations are routinely observed in sunspots across different layers and it is now evident that the umbral flashes and running penumbral waves observed in the chromosphere, and the propagating disturbances observed in the corona are different manifestations of the slow magnetoacoustic waves propagating across these layers. Using high resolution images obtained with the ROSA at a very high cadence we study different characteristics of sunspot oscillations using their power spectra. We also use co-temporal data from SDO and IRIS to find their behaviour at higher layers. Several interesting properties concerning their propagation and dissipation have been revealed which will be discussed in this talk.————————————————————————————————————

Afternoon Session 1 (14:00 - 15:30)

Gianna Cauzzi, INAF Arcetri [14:00 - 14:30]

Heating & Dynamics in the Quiet Chromosphere: The Role of Acoustic Shocks

Most of the magneto-convective energy that drives coronal heating is processed through the chromosphere, yet many questions remain about the dynamics and energetics of this "interface" region, and their connection to the transition region and corona.

In this talk I will focus on one particular aspects of chromospheric dynamics, i.e. acoustic shocks in the quiet (non flaring) Sun. While these shocks are most likely not the dominant source of heating for the outer solar atmosphere, they play an important role in structuring their surroundings, including generating local turbulence and small scale heating, and exerting a strong influence on the dynamics of the lower transition region.————————————————————————————————————

Vasco Henriques, Queen’s University Belfast [14:30 - 14:50]

A proven chromosphere to corona connection via jets in the quiet Sun

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Type II spicules have been shown to reach lower coronal heights by Pereira et al. (2014). Evidence of their on-disk counterparts, RBE and RREs, in the transition region was also found with IRIS in the same work and Rouppe van der Voort et al. (2015). Recently, Henriques et al. (2016) found coronal RBE/RRE counterparts at AIA 304 and AIA 171 using an automated detection method across channels. While some transients across all channels are very obviously related by looking at their overlap, morphology, and temporal coincidence, the automated detection combined with a solid statistical analysis allowed the computation of a minimum value for the percentage of the transients detected that are related across channels (and thus across the chromosphere and the corona). This was achieved by using a combination of Poisson-trial statistics and Chernoff bounds, which were then used to infer the statistical significance of the values, test the null hypothesis, and as a constraint on the parameters of the match criteria. The talk will briefly review the method, as it has the potential to be used in broader sets of noisy data, and will closely analyse particular cases that, besides showing the connection between layers, seem to indicate heating is occurring up to coronal temperatures at heights usually observed in H-alpha. ————————————————————————————————————

David Kuridze, Queen’s University Belfast [14:50 - 15:10]

Kelvin-Helmholtz instability in solar chromospheric jets

Using data obtained by the high resolution CRisp Imaging SpectroPolarimeter instrument on the Swedish 1-m Solar Telescope, we investigate the dynamics and stability of quiet-Sun chromospheric jets observed at disk center.  

Small-scale features, such as Rapid Redshifted and Blueshifted Excursions, appearing as a high speed jets in the wings of the Halpha line, are characterized by short lifetimes and rapid fading without any descending behavior. To study the theoretical aspects of their stability, we model chromospheric jets as twisted magnetic flux tubes moving along their axis, and use magnetohydrodynamic equations to derive the governing dispersion equation. Analytical solutions of the dispersion equation indicate that this type of jet is unstable to Kelvin-Helmholtz instability (KHI). We show that the instability growth time of the detected jets could be very short (few seconds) at the observed high upflow speeds. The generated vortices and unresolved turbulent flows associated with the KHI could be observed as broadening of chromospheric spectral lines. Indeed, the detected structures have enhanced line widths with respect to the background.  Analysis of the energy equation in the partially ionized plasma shows that the ion-neutral collisions may lead to the fast heating of the KH vortices over timescales comparable to the lifetime of chromospheric jets.————————————————————————————————————

Illa R Losada, Stockholm University [15:10 - 15:30]

Formation of sunspots: theory and observations.Sunspots are of basic interest in the solar studies from magnetic fields, as activity counter, to source of coronal mass ejections, flares, and motor of space weather. Still their formation is an unresolved problem in nowadays solar physics. Surface observations depict a 2D structure of the

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spots at the surface, but it is under debate how to infer deep structures and properties from local helioseismology. From the theoretical point of view, flux tubes theory manages to explain some of the observations, but with some drawbacks, like the magnetic field storage mechanism or the survival of a tube rising in a turbulent media.

In this talk I will present another theoretical approach to the formation of sunspots: the negative effective magnetic pressure instability, which is able to concentrate magnetic fields in a turbulent stratified medium. This instability is able suppress turbulence and increase the gas pressure, which drags and concentrate the magnetic fields within. In this framework, sunspots ultimately form within the outermost layers of the Sun. From the observational point of view, I will also present some results and approaches from local helioseismology, where we use Hankel analysis to study the pre-emergence phase of sunspots to try to constraint its deep structures and formation mechanism.————————————————————————————————————

Afternoon Session 2 (16:00 - 17:40)

Richard Morton, Northumbria University [16:00 - 16:30]

Alfvenic waves in the corona

Ground-based measurements of the corona are generally rare and typically restricted to eclipse observations. However, the Coronal Multi-channel Polarimeter (CoMP) offers a fantastic opportunity to observe the corona from the ground, providing imaging spectropolarimetery of infrared Iron lines. One of the surprises from CoMP's high cadence Doppler velocity measurements was the revelation that the corona was replete with Alfvenic waves. I will discuss the recent observations from CoMP and how it contrasts with our understanding of Aflvenic waves in the solar atmosphere, with evidence for counter-propagating waves packets vital for Alfvenic turbulence, connections to Alfvenic waves in solar wind, hints of novel mode-coupling mechanisms and unique applications for measurement of coronal plasma flows.

————————————————————————————————————

Chris Gilbert, University of Colorado (Boulder) [16:30 - 16:50]

Quantifying Line-of-Sight Effects for Spectroscopic Measurements of Alfven Waves and Turbulence in the Solar Corona

There is much debate in the solar community regarding the precise mechanism by which the corona is heated to millions of degrees Kelvin. Alfven waves, driven by fluid motion in the photosphere and propagating upwards to dissipate in the corona, are one of several popular hypotheses for the source of the thermal energy. Observations of off-limb spectral lines are able to constrain some properties of these waves (e.g., amplitudes and phase speeds) as a function of heliocentric altitude. In this work, a forward model is used to simulate plasma properties along thousands of optically thin sightlines over the limb, which are then used to generate spectral lines. This is repeated at many impact parameters, and the resulting statistics are compared to real observations in order to constrain the properties of the Alfven waves.

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————————————————————————————————————

Penny Wu, The University of Delaware [16:50 - 17:20]

Some recent insights into solar wind turbulent dissipation and heating

Solar wind turbulence may be described by magnetohydrodynamics at large scales, but require kinetic description at ion scales in order to include dissipative processes that terminate the cascade. Here kinetic plasma simulations and high-resolution spacecraft observations are compared to facilitate the interpretation of signatures of various dissipation mechanisms. Kurtosis of increments indicates that kinetic scale coherent structures are present, with some suggestion of incoherent activity near ion scales. Conditioned proton temperature distributions suggest heating associated with coherent structures. Further, simulations render that at small turbulence amplitudes the electrons are preferentially heated, whilst at larger amplitudes proton heating is the dominant effect. In the solar wind and corona the protons are typically hotter, suggesting that these natural systems are in the large amplitude turbulence regime.

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Ioannis Kourakis, Queen’s University Belfast [17:20 - 17:40]

Nonlinear waves in non-Maxwellian Space plasmas

www.kourakis.eu

Space plasmas are often characterized by the presence of energetic particles, due to various acceleration mechanisms [1]; this phenomenon is particularly relevant in the solar wind [2], but also in planetary magnetospheres [3] and other environments. In observations, one encounters a distinct power-law dependence of the distribution at high (superthermal) velocity values, which is effectively modelled by a kappa-type distribution function, which reproduces observed data more efficiently that the standard Maxwellian distribution approach [2, 3]. It has been shown from first principles that this ubiquitous superthermal feature of plasmas may alter the propagation characteristics of plasma modes, and modify the plasma screening properties [4-6].

In this short presentation, we shall briefly review, from first principles, the effect of excess electron superthermality on the characteristics of electrostatic nonlinear plasma modes. We employ a kappa distribution function [1] to model the deviation of a plasma constituent (electrons, in general) from Maxwellian equlibrium. It is shown that an excess in superthermal propulation (i.e. a small value of the kappa index) modifies the charge screening mechanism, affecting the dispersion laws of both low- and higher frequency electrostatic modes substantially. This may be useful in Space “experimental” diagnostics, as various observations are interpreted as manifestations of electron superthermality [4-6]. The effect of superthermality on their propagation dynamics (existence laws, stability profile) of solitary waves is also briefly addressed [6].

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[1] V.M. Vasyliunas, J. Geophys. Res. 73, 2839 (1968).[2] V.Pierrard and M. Lazar, Solar Phys. 267, 153 (2010).[3] P. Schippers et al, J. Geophys. Res. 113, A07208 (2008).[4] M. Hellberg et al, J. Plasma Physics 64, 433 (2000).[5] Mike Hapgood et al, Planet. Space Sci. 59, 618 (2011).[6] S. Sultana, I. Kourakis, N.S. Saini, M.A. Hellberg, Phys. Plasmas 17, 032310 (2010); S. Sultana and I. Kourakis, Plasma Phys. Cont. Fus. 53, 045003 (2011);S. Sultana, G. Sarri and I. Kourakis, Phys. Plasmas 19, 012310 (2012);I. Kourakis, S. Sultana & M.A. Hellberg, Plasma Phys. Cont. Fusion, 54, 124001 (2012); G. Williams and I. Kourakis, Plasma Phys. Cont. Fusion 55, 055005/1-13 (2013).————————————————————————————————————

FINISH

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School & Workshop VenuesStudents will stay in the Elms Village Halls of residence. This is along the Malone Road and is map point 38 on the attached map. This is approximately 1.3km from the School & Workshop venues. Students must report to the reception at the Elms Village to get their key card and room. The reception is the building beside the barrier as you enter the site. Breakfast will be served in the Tree House every morning from 7am to 10am.

The school will be held in the QUB Canada Room and Council Chamber in the Lanyon Building (main Queen’s building). This is map point 1 in the attached map. It is up the stairs as on the left as you enter the Lanyon building from the front end (University Road Entrance).

The workshop will take place at the Emeleus Lecture Theatre. This is in the archway at map point 1s in the map below.

A pdf version of the map can be found here: http://titus.phy.qub.ac.uk/docs/qubmap.pdf

Social EventsDrinks reception at 17:30 Thursday 25th August

Informal gathering at Cutters Wharf at 19:00 Tuesday 30th August (Dinner will be provided, but not drinks).

Conference dinner at 19:00 on Wednesday 31st August 2016 - QUB Great Hall

Prof. Francis Keenan’s “The Science of Science-Fiction” lecture: TBD

Tourist InformationThe weekend (27th & 28th August) is free of lectures. Therefore, any students looking for tourist information should find it at one of these web sites:

http://visitbelfast.com/

http://www.discovernorthernireland.com/

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Queen’s Campus Map

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Directions from Queen’s to Cutters Wharf

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