Diapositive 1 - Institut d'études scientifiques de Cargèse (IESC)

Diapositive 1 - Institut d'études scientifiques de Cargèse (IESC) Diapositive 1 - Institut d'études scientifiques de Cargèse (IESC)

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2013 29 Avril 8 mai COSMIC ACCELERATORS Diego Götz CEA – Sce Astrophysique 91191 Gif / Yvette France 01 69 08 59 77 Diego.gotz@cea.fr Direction scientifique : Giovanna Chimini Contact : Dominique Donzella tél : 04 95 26 80 40 www.iesc.univ-corse.fr

2013

29 Avril

8 mai

COSMIC ACCELERATORS

Diego Götz

CEA – Sce Astrophysique

91191 Gif / Yvette

France

01 69 08 59 77

Diego.gotz@cea.fr

Direction scientifique :

Giovanna Chimini

Contact :

Dominique Donzella

tél : 04 95 26 80 40

www.iesc.univ-corse.fr

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Abstract Booklet

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Lectures .......................................................................................................................................... 4

Oral Presentations ...................................................................................................................... 8

Poster Contributions ............................................................................................................... 13

Schedule ...................................................................................................................................... 23

List of Accepted Applicants ................................................................................................... 24

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Lectures

• Acceleration on all scales (introduction to the school): Felix Aharonian (DE,IE)

The intention of this talk will be the discussion of high-‐energy non-‐thermal phenomena

on all scales, which will include a general discuss of particle acceleration in different

astrophysical environments. The discussion will have a phenomenological character

without details on acceleration mechanisms, which will be covered in other talks. On the

other hand, it will be discuss the non-‐thermal phenomena in general, and particle

acceleration in particular in the context of relativistic outflows, including jets of different

scales

• Radiative Processes I (non thermal): Alexandre Marcowith (FR)

Non-‐thermal radiations are ubiquitous in sites of acceleration of energetic particles to

high energies. The lecture will provide a rather exhaustive review of these processes

and illustrate them with some particular relevant astrophysical cases. Both compact

objects and diffuse environments will be discussed.

• Radiative processes II (thermal): Jelle Kaastra (NL)

The lecturer will present the basics of high-‐resolution X-‐ray spectroscopy. After a brief

summary of atomic structure, the basic processes related to emission and absorption in

a plasma are introduced. Examples that are encountered frequently are presented but

also some challenging diagnostics that will become available with future instruments

are described.

• Acceleration Processes I (Fermi I): Andrei Bykov (RU)

Particle acceleration by collisionless shocks waves (Fermi I type acceleration) is proved

to be the most efficient mechanism of relativistic particle production in many

astrophysical objects with high-‐energy release -‐ supernova remnants, stellar winds, jets

etc. The high efficiency of particle acceleration implies the importance of non-‐linear

feedback effects connecting self-‐generated fluctuating magnetic fields and non-‐thermal

particles. These lectures will review the current status and perspective of the Fermi I

mechanism in connections with high-‐energy astrophysics.

• Acceleration Processes II (Fermi II and Monte Carlo): Don Ellison (USA)

There is substantial evidence that magnetic fields can be strongly amplified in some

astrophysical sources. The stronger the magnetic field, the more important second-order

Fermi particle acceleration becomes as particles scatter off the strong magnetic

turbulence. The lecturers will discuss how the predictions of second-‐order Fermi

acceleration differ from those of the more widely used first-‐order Fermi mechanism and

emphasize the application to cosmic-‐ray production in young supernova remnants.

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

• Acceleration Processes III (Magnetic reconnection, Charge separation, Poynting

Fluxes, rotating B Fields, Jets): Henk Spruit (DE)

Introduction to magneto-‐hydrodynamics (MHD) with emphasis on processes of flow

acceleration by magnetic fields, the interpretations of the Poynting flux in MHD. As a

practical application of MHD this will be followed by the rotating magnetic field model

for the acceleration of astrophysical jets, including Poynting flux conversion into kinetic

energy, the collimation of jets, and finally the role of internal instabilities of the magnetic

field in jets in the dissipation of magnetic energy, and their contribution to flow

acceleration.

• AGNs: Volker Beckmann (FR)

Active Galactic Nuclei provide particle accelerators that produce confined jets up to

distances of 100 kpc and more. This lecture will discuss the current status of AGN

research, with a special emphasis on AGN displaying jets. What types of AGN can become

strong particle accelerators? How does the AGN interact with its environment and how

did the AGN population evolve on cosmological time scales? The lecture will then focus

on the emission processes we observe in blazar jets. Here we can study the physical

processes, such as synchrotron self-‐Compton and external Compton processes. In radio

galaxies we can directly observe spatial components, or "blobs", as they are being

emitted and then as they travel downstream. Shocks and knots in the jet have been

identified and sensitive observations in other wavebands allow us to correlate

morphological evolution in the radio to the multi-‐wavelength light curves. But the main

question still persists: how are the jets formed in the first place? This question is tightly

connected to the accretion process powering the AGN and the central (Kerr?) black hole.

• SNRs: Jacco Vink (NL)

For a long time supernova remnants have been thought to be the main contributors to

the observed cosmic-‐ray flux below 3x10 15 eV. Since 20 years the amount of evidence

that this is indeed the case has rapidly increased. Recent gamma-‐ray and X-‐ray

observations inform us that particles are accelerated at least up to 100 TeV, and there is

evidence that a significant amount of kinetic energy is converted to cosmic-‐ray energy.

Nevertheless, the final evidence of particles with energies approaching 3x10 15 eV is still

lacking, and also the evidence that more than 10% of the SNR energy is in cosmic rays is

still not secure. The lecturer will discuss the observational situation and what remains

to be done in the future.

• PWNe: Elena Amato (IT)

These lectures will provide a review of the current status of our knowledge on Pulsar

Wind Nebulae. The lecturer will mostly be concerned with their role as cosmic ray

factories. They are natural sources of leptonic anti-‐matter and also the only class of

astrophysical objects for which we have direct evidence of particle acceleration up to

PeV energies. The lecturer will summarize what we understand of the processes through

which the rotational energy of the central pulsar is first converted into a highly

relativistic magnetized wind and then into acceleration of particles up to the highest

energies achieved in the Galaxies.

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

• GRBs: Frederic Daigne (FR)

Gamma-‐ray bursts are bright transient phenomena associated to ultra-‐relativistic

outflows ejected by newborn compact sources. The lecturer will review the main

observations and our current physical understanding of these phenomena. Then the

lecturer will discuss particle acceleration in GRBs: (i) acceleration of the particles

responsible of the observed gamma-‐ray emission; (ii) acceleration of hadrons and

possible signatures in gamma rays or neutrinos; (iii) possible acceleration of ultra-‐high

energy cosmic rays.

• Simulations: Lorenzo Sironi (USA)

The lecturer will discuss recent progress in our understanding of collisionless

astrophysical shocks, thanks to powerful ab initio plasma simulations. Fully kinetic

particle-‐in-‐cell (PIC) simulations simultaneously capture the kinetic physics of electrons,

whose emission powers the radiative signature from astrophysical sources, and of

protons, that regulate the shock dynamics and evolution. In hybrid simulations, where

only protons are treated kinetically (here, electrons constitute a massless charge-neutralizing

fluid), the shock evolution can be followed up to much longer times than in

PIC simulations, thus approaching the time and length scales most relevant to

astrophysics. Thanks to recent advances in numerical algorithms and computer

capabilities, PIC and hybrid simulations have allowed major progress in our

understanding of the physics of shock formation, magnetic field generation, and particle

acceleration, thus contributing to unveil the nature of the most powerful astrophysical

sources.

• Cosmic Rays I (galactic): Vladimir Ptuskin (USA)

The lecturer will discuss the processes of cosmic-‐ray acceleration and propagation in the

Galaxy. Discussion includes the acceleration in supernova shocks, the nature of “knee” in

cosmic ray spectrum at energy 3 PeV, the transition from galactic to extragalactic

component, the collective effects of cosmic rays in the Galaxy.

• Cosmic Rays II (extragalactic): Martin Lemoine (FR)

The origin of cosmic rays with energy E> 10 18 eV represents a long-‐standing problem in

astrophysics, even though the development of gigantic detectors has brought in key

experimental results. This course will discuss offer an introduction to the physics and

the astrophysics of ultra-‐high energy cosmic rays. It will first discuss the recent

experimental results, then it will discuss the physics of acceleration in powerful

astrophysical sources and the physics of transport in the intergalactic medium; finally it

will discuss the significance of recent experimental results and the prospects for future

detectors.

• Isolated Neutron Stars: Andrea De Luca (IT)

Isolated Neutron Stars (INS) are supposed to host the most extreme physical conditions

existing in the local universe. 45 years of multi-‐wavelength astronomy unveiled a

complex and rich phenomenology, which led to a classification into different "species".

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

First, the lecturer will review and discuss such "INS diversity", pointing to actual

genetic/evolutionary differences, possibly related to the INS' gigantic, rotating magnetic

fields. Then, the lecturer will focus on INS as strong emitters of non-‐thermal

electromagnetic radiation, originating from charged particles accelerated in their

magnetospheres, at the expense either of their rotational energy reservoir, or of the

decay of an ultra-‐high magnetic field.

• HE Binaries: Guillaume Dubus (FR)

Observations of high-‐energy gamma-‐ray emission offer new insights into non-‐thermal

processes in binaries. The lecturer will explain what the observed variability and orbital

modulations tell us about the origin of the high-‐energy particles. In addition the lecturer

will present the challenges that models currently face and discuss the consequences on

our understanding of pulsar winds, relativistic jets and colliding stellar winds.

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Oral Presentations

1. J. Heyl

Cosmic rays from pulsars and magnetars

We compare the expected abundance of cosmic ray electrons and positrons from pulsars

and magnetars. We assume that the distribution of infant pulsars and magnetars follows

that of high-‐mass stars in the Milky Way and that the production rate of cosmic rays is

proportional to the spin-‐down and magnetic-‐decay power of pulsars and magnetars,

respectively. In combination with primary and secondary cosmic ray leptons from other

sources (especially supernova remnants), we find that both magnetars and pulsars can

easily account for the observed cosmic ray spectrum, in particular the dip seen by HESS

(High-‐Energy Stereoscopic System) at several TeV and the increase in positron fraction

found by PAMELA (Payload for Antimatter Exploration and Light Nuclei Astrophysics).

Co-‐authors : Gill, Ramandeep, Hernquist, Lars

2. B. Khiali

Non-‐thermal Emission from the Accretion-‐Disk/Coronae of AGNs and Particle Acceleration

by Magnetic Reconnection

High energy particles are ubiquitous in astrophysical environments and the origin of

ultra high energy cosmic rays (UHECR) is still an open question. Likewise, very high

energy observations of active galactic nuclei (AGNs) and gamma ray bursts (GRBs) with

the Fermi and Swift satellites and ground based gamma ray experiments (HESS,

VERITAS and MAGIC) are challenging current theories of particle acceleration, mostly

based on the acceleration in shocks, which try to explain how particles are accelerated

to energies above TeV in regions relatively small compared to the fiducial scale of their

sources. It is usually assumed that the emitting high energy particles are accelerated to a

power-‐law distribution at relativistic shocks, via the so-‐called Fermi mechanism in

shocks. Recent magneto-‐hydrodynamics (MHD) studies have revealed that particle

acceleration in magnetic reconnection sites can be rather efficient since a 1st order

Fermi process can occur there too. In this talk, we discuss this acceleration mechanism

in the framework of AGNs, considering that magnetic reconnection events can be very

frequent in the inner regions of the corona of the accretion disks, or in the jets. We

compute the corresponding acceleration rate and the relevant loss rates in order to

reproduce the observed high energy spectrum of different classes of AGNs. We consider

both leptonic and hadronic models and compare the efficiency of such acceleration

processes with alternative acceleration mechanisms.

Co-‐authors: E. M. de Gouveia Dal Pino, M.V. del Valle, G. Kowal, Helene. Sol

3. D. Onic

Multiwavenegth analysis of supernova remnant 3C396

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

The radio spectrum of 3C396 shows both a low-‐frequency turnover and flattening at

higher frequencies. This SNR has flat radio spectral index (below 0.5) which is one of the

characteristic of SNRs that expand in high density environments and interact with

molecular clouds. Recently, interaction with molecular cloud is detected for this

remnant. Possible explanations for flat spectral index observed in this SNR as well as the

discussion on the Fermi-‐LAT observations in the direction of this remnant will be

presented.

4. J. Joshi

Testing hadronic models of gamma ray production at the core of Cen A

Pierre Auger experiment has observed a few cosmic ray events above 55 EeV from the

direction of the core of Cen A. These cosmic rays might have originated from the core of

Cen A. High energy gamma ray emission has been observed by HESS from the radio core

and inner kpc jets of Cen A.

We are testing whether pure hadronic interactions of protons or heavy nuclei with the

matter in the core region or photo-‐disintegration of heavy nuclei can explain the cosmic

ray and high energy gamma ray observations from the core of Cen A. The scenario of p-gamma

interactions followed by photo-‐pion decay has been tested earlier by Sahu et al.

(2012) and found to be consistent with the observational results. In this paper we have

considered some other possibilities (i) the primary cosmic rays at the core of Cen A are

protons and the high energy gamma rays are produced in p-‐p interactions,(ii) the

primary cosmic rays are Fe nuclei and the high energy gamma rays are produced in Fe-‐p

interactions and (iii) the primary cosmic rays are Fe nuclei and they are photo-disintegrated

at the core. The daughter nuclei de-‐excite and high energy gamma rays are

produced.

The high energy gamma ray fluxes expected in each of these cases are compared with

the flux observed by HESS experiment to normalise the spectrum of the primary cosmic

rays at the core. We have calculated the expected number of cosmic ray nucleon events

between 55 EeV and 150 EeV in each of these cases to verify the consistencies of the

different scenarios with the observations by Pierre Auger experiment. We find that if the

primary cosmic rays are Fe nuclei then their photo-‐disintegration followed by de-excitation

of daughter nuclei may explain the observed high energy particle emissions

from the core of Cen A. The luminosity of the cosmic ray Fe nuclei required to explain

the observational results of HESS and Pierre Auger is higher than the luminosity of the

cosmic ray protons in the p-‐gamma interaction model. The required cosmic ray

luminosity depends on the density of the low energy photons at the source which photo-disintegrate

the Fe nuclei and the size of the emitting region.

Co-‐authors: Nayantara Gupta

5. I. Vovk

Variability of gamma-‐ray emission from blazars on the black hole timescales

We investigate the variability properties of blazars in the GeV band using the data of the

Fermi/LAT telescope. We find that blazars exhibit variability on the scales down to the

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

minimal timescale resolvable by Fermi, which is a function of the peak photon count rate

in the LAT. This implies that the real minimal variability timescales for the majority of

blazars are typically shorter than those resolvable by the LAT. We find that for several

blazars these minimal variability timescales reach those associated to the blazar central

engine, the supermassive black hole. At the same time, none of the blazars exhibits

variability on the timescale shorter than the black hole horizon light crossing time

and/or the period of rotation around the last stable circular orbit. Based on this fact, we

argue that the timing properties of the gamma-‐ray signal could be determined by the

processes in the direct vicinity of the supermassive black hole

Co-‐authors: A. Neronov

6. G. Vila

Proton loading of relativistic jets

Relativistic neutrons are injected in the corona surrounding an accreting black hole

through hadronic interactions of locally accelerated protons. A fraction of these

neutrons may escape and penetrate the base of the jet, later decaying into protons. This

is a possible mechanism for baryon loading of Poynting-‐dominated outflows. We study

the characteristics of the proton distribution and the impact on the radiative spectrum

of the jet. We also investigate the fate of those neutrons that escape the corona into the

external medium.

Co-‐authors: Florencia L. Vieyro & Gustavo E. Romero

7. K. Auchetti

Fermi-‐LAT observations of Galactic supernova remnants Kesteven 78 and Kesteven 79.

Observational evidence from thermal and non-‐thermal emission of supernova remnants

(SNRs) has provided increasing support in favour of cosmic ray (CR) acceleration at

their rapidly-‐expanding shock fronts. Accelerated charged particles lose their energy via

a number of different mechanisms and the production of gamma-‐ray emission can be a

diagnostic signature of these processes. Whether this gamma-‐ray emission is hadronic

or leptonic in nature is currently a hotly debated topic in the literature. SNRs known to

be interacting with molecular clouds from the detection of 1720 MHz hydroxyl (OH)

masers, provide effective targets for detecting and studying hadronic gamma-‐ray

emission. We report on the detection of gamma-‐ray emission coincident with Galactic

SNRs, Kesteven 78 and Kesteven 79, that are known to be interacting with nearby

molecular clouds. We use ~52 months of data from the Large Area Telescope on board

the Fermi Gamma-‐ray Space Telescope and perform a detailed spatial and spectral

analysis of the Fermi-‐LAT observations in the regions of these SNRs. This analysis allows

us to constrain the origin of the gamma-‐ray emission as observed in these remnants.

Co-‐authors: Dr. Pat Slane (SAO) and Dr. Daniel Castro (MIT)

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

8. Y. Yuan

Modeling Gamma-‐ray Flares in the Crab Nebula

The gamma-‐ray emission from the Crab Nebula shows variations on a wide range of

time scales, with the most dramatic events being the flares observed by Fermi and

AGILE: the flux can increase by a factor of ~10 within ~10 hours; the spectrum is

characterized by a peak energy ~300 MeV, while no variation in other wavebands was

detected. These variations present a great challenge to particle acceleration mechanisms.

We consider two possible explanations of these flares. Firstly, we consider emission

from a moving relativistic shock terminating the pulsar wind. Secondly, we treat the

pulsar and its wind as a current generator and supposing that the current filaments into

individual pinches that can undergo radial collapse and become strongly dissipative

when the electric field becomes as strong as the magnetic field and Larmor radius of the

highest energy particles becomes comparable with the radius. The application of these

models to pulsar wind nebulae and relativistic jets will be outlined.

Co-‐authors: Roger Blandford, Paul Simeon

9. T. Antecki

Stochastic acceleration of suprathermal particles under pressure balance conditions

The acceleration of suprathermal charged particles in the heliosphere under pressure

balance conditions including for the first time the radial spatial particle diffusion and

convection in the solar wind is investigated. The physical conditions are derived for

which the stationary phase space distribution of suprathermal particles approaches the

power-‐law distribution f ∝ p^(−5), which is often seen in spacecraft observations. For

separable source distributions in momentum and position we analytically solve the

stationary particle transport equation for a radially constant solar wind speed V_0 and a

momentum-‐independent radial spatial diffusion coefficient. The resulting stationary

solution at any position within the finite heliosphere is the superposition of an infinite

sum of power laws in momentum below and above the (assumed mono-‐momentum)

injection momentum p_I . The smallest spatial eigenvalue determines the flattest power

law, to which the full stationary solution approaches at large and small enough momenta.

Only for the case of a reflecting inner and a free-‐escape outer spatial boundary, one

small eigenvalue exists, yielding the power-‐law distribution f ∝ p^(−5) at sufficiently

large momentum values. The other three spatial boundary conditions imply steeper

momentum spectra. Momentum spectra and radial profiles of suprathermal particles are

calculated by adopting a uniform outer ring spatial source distribution.

Co-‐authors: R. Schlickeiser, M. Zhang

10. S. De Jong

M87 in hard X-‐rays

The nearby (D=16 Mpc) FRI radio galaxy M87 is one of the best studied examples of a

gamma-‐ray bright radio galaxy.

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

While in the X-‐ray band below 10 keV, the nucleus of this source shows strong

variability, the source does not seem to be detectable in the hard X-‐ray domain by e.g.

Swift or INTEGRAL. Since extrapolating Chandra data indicates that at least during some

periods significant hard X-‐ray emission takes place, we investigate 1.7 Ms of INTEGRAL

IBIS/ISGRI data in order to establish the best upper limit in this energy range to date. In

the energy band 20-‐60 keV we find an average upper limit of f2.9) to connect the hard

and soft X-‐ray fluxes.

Together with data from other wavelengths, including Fermi/LAT, we investigate the

broad-‐band spectral energy distribution of M87. Since M87 has been detected in the TeV

band, combined with the steep power law between hard and soft X-‐rays, we argue that

the SED of M87 might be modeled similarly to a high-‐peaked BL Lac (HBL), which is a

low luminosity blazar.

Co-‐authors: V. Beckmann, S. Soldi, F. Mattana, J.A. Zurita Heras

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Poster Contributions

1. S. Lecoz

Microwave detection of extensive air shower at the Pierre Auger Observatory

Spreading over 3000km² in the Argentina pampa, the Pierre Auger Observatory is the

greatest cosmic rays detector worldwide. It observes the extensive air shower (EAS)

produced by the cosmic ray interactions in the atmosphere, with surface detectors and

fluorescence telescopes. The electromagnetic content of the EAS is at the origin of

different types of electromagnetic wave emissions, in different wavelength ranges. Air

shower microwave emission has been observed by few beam experiments. The Pierre

Auger Observatory develops microwave detectors to obtain valuable observables

related to the EAS, with three different projects: MIDAS (Microwave Detection of Air

Shower), AMBER (Air shower Microwave Bremsstrahlung Experimental Radiometer),

and EASIER (Extensive Air Shower Identification using Electron Radiometer). AMBER

and MIDAS are microwaves telescopes, EASIER consists of 61 antennas set on 61 surface

detectors. AMBER and EASIER are triggered by the surface detectors while MIDAS has

his own trigger. The status of these projects will be reported.

2. M. Pavlovic

The radio surface brightness to diameter relation for galactic supernova remnants

We present new empirical radio surface brightness-‐to-‐diameter (Σ–D) relations for

supernova remnants (SNRs) in our Galaxy. We also present new theoretical derivations

of the Σ–D relation based on equipartition or on constant ratio between cosmic rays and

magnetic field energy. A new calibration sample of 60 Galactic SNRs with independently

determined distances is created. Instead of (standard) vertical regression, used in

previous papers, different fitting procedures are applied to the calibration sample in the

log Σ– log D plane. Non-‐standard regressions are used to satisfy the requirement that

values of parameters obtained from the fitting of Σ–D and D–Σ relations should be

invariant within estimated uncertainties. We impose symmetry between Σ–D and D–Σ

due to the existence of large scatter in both D and Σ. Using four fitting methods that treat

Σ and D symmetrically, different Σ–D slopes β are obtained for the calibration sample.

Monte Carlo simulations verify that the slopes of the empirical Σ–D relation should be

determined by using orthogonal regression because of its good performance in data sets

with severe scatter. The slope derived here (β = 4.8) is significantly steeper than those

derived in previous studies. This new slope is closer to the updated theoretically

predicted surface-‐brightness–diameter slope in the radio range of the Sedov phase. We

also analyze the empirical Σ–D relations for SNRs in a dense environment of molecular

clouds and for SNRs evolving in the lower-‐density interstellar medium. Applying new

empirical relations to estimate distances of Galactic SNRs results in a dramatically

changed distance scale.

3. M. Grudzinska

TeV radiation from binaries

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

VHE radiation from binaries shows a very comlpex phenomenology. I will review the

current observations of binaries in the TeV range. I will present the models of formation

high energy gamma rays in binaries and compare the theoretical models with

observations.

Co-‐autohrs: T. Bulik, B. Rudak

4. H. Jermak

Monitoring the optical polarization of blazars with RINGO2 on the Liverpool Telescope

I will introduce the Liverpool Telescope blazar programme -‐ an optical imaging

polarization study of a sample of radio-‐loud blazars using the rapid-‐response RINGO2

polarimeter on the world's largest fully autonomous robotic optical telescope. The

blazars are monitored routinely both in quiescence and during flare events. I will

describe the polarimeter and discuss the blazar sample, along with looking toward the

future with Liverpool's upcoming multi-‐colour imaging polarimeter, RINGO3.

Co-‐authors: Carole Mundell, Iain Steele

5. B. Rani

Broadband spectral modeling of BL Lac object S5 0716+714

Densely time sampled multi-‐frequency flux measurements of the extreme BL Lac object

S5 0716+714 over the past four years allow us to study its broad-‐band variability,

allowing us to look into the detailed physics, with emphasis on the location and size of

the emitting regions and the evolution with time. In this talk, I will briefly discuss the

details and limitations of one-‐zone synchrotron-‐self Compton model.

Co-‐authors: T. P. Krichbaum, L. Fuhrmann, M. Bottcher, B. Lott

6. I. Babyk

Gamma Ray Flare from PSR B1259-‐63/LS 2883

PSR B1259-‐63/LS 2883 is a boundary system, where a 47.7 ms pulsar orbits a luminous

star in a very eccentric orbit (e=0.87, period P=1237). The recent observations of PSR

B1259-‐63/LS 2883 with Fermi/LAT revealed a complex behaviour of the system in GeV

gamma rays. Near to the periastron passage, the source has an energy flux 6 x 10^-‐11

erg cm^-‐2 s^-‐1, but a month after periastron passage a "surprise" flare has been

detected with level of 3 x 10^10 erg cm^-‐2 s-‐1.

Co-‐authors: M. Chernyakova (DIAS, DCU)

7. T. Oceguera

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

On detector calibration and characterization “High Altitude Water Cerenkov (HAWC)” in

the phase HAWC100 .

The High Altitude Water Cherenkov (HAWC) Observatory is a TeV gamma ray detector

currently under construction at Sierra Negra in Mexico. HAWC will utilize the wide-angle,

high duty cycle water Cherenkov technique developed by Milagro, but use new

technology, a larger detection area, and higher altitude to improve sensitivity by an

order of magnitude. HAWC will survey the TeV gamma ray sky, measure spectra of

galactic sources up to and beyond 100 TeV, and map galactic diffuse gamma ray

emission. With its wide field of view and continuous operation, HAWC will also be a

powerful instrument with which to study transient phenomena. HAWC will have

significant overlap with space and ground-‐based detectors like NASA-‐FERMI, MAGIC,

HESS, AUGER and ICECUBE. The amount of information will be handled in the order of

Peta-‐bytes, so for processing and storage technologies are used characteristic of high

performance computing (parallel processing, multi-‐threads). The student will contribute

through simulations the performance of the instrument and analysis of data obtained by

Monte Carlo techniques and simulate the performance of the detector at various stages.

Will generate cascades of product particles from collisions of cosmic rays with the

atmosphere. These simulations will be compared with data taken with the HAWC30 to

start the installation phase HAWC100. Will develop models of noise and will subtracting

this method as background noise to the signal recorded by HAWC.

8. I. Rodriguez Barrera

CHARACTERIZING MAGNETIZED ATMOSPHERIC IN VERY LOW-‐MASS OBJECTS

The dust clouds play an important role in the atmospheres of very low-‐mass objects

such as Brown Dwarfs, Gas Giant planets and M-‐Dwarfs. Clouds represent an important

opacity source (backwarming due to strong dust opacity). If a localised volume of the

atmosphere is ionised, hence maybe constituting a plasma, this would significantly alter

the subsequent gas-‐plasma chemistry and introduce a menagerie of plasma processes.

Co-‐authors: Ch. Helling, C. R. Stark and P. Rimmer

9. M. Fouka

Light Curves of GRB's afterglow with High Latitudes arrival time delay

Light curves of GRB's afterglow have been computed by taking into account high

latitudes arrival time delay, in spherical geometry. To this aim, we have adopted Feng et

al. (2002) model for describing the fireball hydrodynamical evolution. For the later, we

consider an evolving radiative efficiency. Besides, the optically thin synchrotron is

assumed to be the main radiative process. Results are compared to XRT/Swift light

curves and to some R-‐band optical light curves.

Co-‐authors: S. Ouichaoui

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

10. J.C. Leyder

When stellar winds collide: high-‐energy emission unveils the physics of massive stars

Massive stars have strong stellar winds, high mass-‐loss rates, and extreme terminal

wind velocities. When two such objects are orbiting each other, it may lead to a

colliding-‐wind binary system. In that case, the system has excess X-‐ray emission which

stems from the hydrodynamical shocks that form between their stellar winds, in

addition to the intrinsic X-‐ray emission from both stars. Thanks to particle acceleration

taking place in those shocks, non-‐thermal emission in the high-‐energy domain is

expected.

11. C. Borwankar

Recent results from TACTIC telescope

I will present some recent results from TACTIC (TeV Atmospheric Cherenkov Telescope

with Imaging Camera) , with dish size 3.5 m diameter, working in energy range of 1 TeV

to 16 TeV , situated at Mount Abu, India. I will also talk about the present status of the

MACE telescope,with dish size of 21 m diameter expected to work in 20 GeV to 10 TeV

energy range, being set up at Hanle, India.

12. M. Supsar

Plasma instabilities in fast pair beams in cosmic voids

The interaction of TeV gamma rays from distant blazars with the extragalactic

background light produces relativistic electron-‐positron pair beams by the photon-‐

photon annihilation process. The created pair beam distribution is unstable to linear

two-‐stream instabilities of both electrostatic and electromagnetic nature in the

unmagnetized intergalactic medium (IGM). The maximum electrostatic growth rate

occurs at angles of 39fdg2 with respect to the pair beam direction, and is more than

three orders of magnitude greater than the maximum Weibel growth rate, indicating

that the linear oblique electrostatic instability operates much faster than the Weibel

instability. The dissipation of the generated electrostatic turbulence is different for

intense and weak gamma-‐ray blazars. For intense blazars, the normalized number of

generated pairs n 22 = nb /[10–22 cm–3] exceeds the critical density nc (T) = 4.8 × 10–3

T 4 for given normalized IGM temperature T 4 = T/[104 K] necessary for the onset of the

modulation instability, so that all free kinetic pair energy is dissipated in heating the

IGM in cosmic voids. For weak blazars, half of the initial energy density of the beam

particles is transferred to the electrostatic and electromagnetic fluctuations on

timescales smaller than the inverse Compton energy loss timescale of the pairs. In both

cases, this prevents the development of a full electromagnetic pair cascade as in vacuum.

For weak blazars, the superluminal electrostatic fluctuations are dissipated by the

inverse Compton scattering into transverse electromagnetic waves by the relaxed

relativistic pair particles to optical frequencies, implying the occurrence of optical

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

electrostatic bremsstrahlung pair halos from weak blazars with spectral flux densities

below 50 μJy.

Co-‐authors: R. Schlickeiser, D. Ibscher

13. K. Malanchev

Non-‐stationary disk accretion in X-‐ray Novae

In this work light curves of soft X-‐ray transients are studied. We assume that on the first

stage of disk accretion all the hydrogen is ionized and the disk size is constant. The zone

of partically ionized hydrogen appears on the outer edge of the disk 30÷70 days after X-ray

maximum. Convection, appeared in this zone, increases viscosity parameter and

accretion rate. In this case secondary peak appears on the light curve. On the next stage

of accretion the edge between neutral hydrogen and completely ionized hydrogen

moves to the inner edge of the disk. Fitting both X-‐ray and optical light curves of X-‐ray

transient one could determine a coupe of parameters of this object: alpha parameter

value before and after the secondary peak, mass of black hole and its Kerr parameter.

Co-‐authors: A. V. Meshcheryakov, N. I. Shakura

14. C. Tchernin

Neutrino signal from extended Galactic sources in IceCube

The Galactic Plane is the brightest source of gamma rays on the sky. It should be also

(one of the) brightest very-‐high-‐energy neutrino sources, since neutrino flux equal to

the gamma-‐ray flux is produced by the cosmic ray interactions in the interstellar

medium.

In this work, we investigate if the neutrino flux from the entire Galactic Plane or from a

part of it is detectable by the IceCube detector in a reasonable exposure time.

Co-‐authors: Andrii Neronov, J. Aguilar and T. Montaruli

15. A. Araudo

Jets from massive protostars as efficient (non-‐relativistic) cosmic accelerators

There is evidence supporting that the evolution of protostars goes through different

phases including accretion of matter onto the central protostar with the formation of a

circumstellar disk and bipolar jets. The non-‐thermal radio emission claimed to be

detected from several young stellar object jets in the last years has been confirmed very

recently, after the detection of linearly polarized radio emission from the famous HH80-‐

81 protostellar jet. The polarization pattern of the HH80-‐81 jet is strikingly similar to

that of AGN jets, that are efficient cosmic-‐ray accelerators and gamma-‐ray emitters. We

study the acceleration of particles in (internal and terminal) shocks produced in fast

protostellar jets. A population of relativistic particles in the complex environment of the

massive molecular cloud where the protostar is being formed will produce high-‐energy

radiation through a variety of processes. We compute the non-‐thermal emission, from

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

radio to gamma-‐rays, but focus on the high-‐energy part of the spectrum. We conclude

that jets from massive protostars are a new kind of cosmic accelerators and gamma-‐ray

sources.

Co-‐authors: Luis Felipe Rodriguez

16. A. Dumas

Indirect search for Dark Matter in nearby Dwarf Spheroidal Galaxies with ANTARES

After a short introduction about dark matter and ways to detect it, I will explain the

astrophysical factor J and some density profile of dark matter in dwarf galaxies. In a last

part, I will present some differential spectra of neutrinos product by differents channels

of dark matter annihilation.

17. T. Vuillaume

Anisotropic emission in the vicinity of an accretion disk

The gamma ray emission of AGNs is thought to arise redominantly from Inverse

Compton Scattering of low energy photons by relativistic leptons, but the exact source

and location of these photons is still a matter of discussion. For BL Lac type objects , the

main contribution is probably provided by synchrotron radiation and the high energy

emission is thus dominated by Synchrotron Self Compton(SSC) process. For luminous

quasars however, the emission from the accretion disc and the reprocessed components

(Broadlines and molecular torus) is probably significant and can even be dominant.

Whereas diffuse component is approximately isotropic, the emission from the accretion

disc is highly anisotropic and the effect on Inverse Compton emission can be very

important.

18. S. Vaupre

Cosmic-‐ray Interaction with Molecular Clouds

Recent results of observation and modelisation of a molecular cloud ionized by cosmic

rays from the nearby super-‐nova remnant W28.

Co-‐authors: Cecilia Ceccarelli, Pierre Hily-‐Blant, Guillaume Dubus, Thierry Montmerle

19. K. Ghezali

Gamma ray emission and pairs e-‐e+ cascades in binary systems

The study of the spectral shape and variability of the gamma emission inform us about

the geometry and the nature of the emitting region. I'm particularly interested by binary

gamma which are VHE sources and constituted of a stellar mass compact object (black

hole or neutron star) orbiting around a massive star hot type O, B or Wolf-‐Rayet. In

many of these binarys, there is a modulation of the emission of gamma in function of

orbital phase of the binary system. We think that this modulation is due, at least in part,

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

to the absorption of gamma photons in the intense radiation field of the companion star.

Knowing the spectral type of the star, we can easily estimate the probability of

absorption along the line of sight which varies with orbital phase. The electron-‐positron

pairs formed by absorption of gamma photon is very energetic and they can even

interact with the stellar photon fields by inverse Compton to form new gamma photons.

These new gamma photons can perform a certain distance of the star befor eventually

being absorbed in their turn. So, by this processus, a three-‐dimensional electromagnetic

cascads is developed. The modelisation of these cascades and other associated emission

process is a way to probe the environment of the compact object on astronomical unit

scales order which are intermediate between the immediate vicinity of the compact

object studied by X-‐ray and radio emission observed in distant flux or relativistic winds.

20. B. Olmi

Modeling the Crab Nebula non-‐thermal emission by numerical simulations

A set of two-‐dimensional axisymmetric relativistic magnetohydrodynamic simulations

has been developed, optimized for the Crab Nebula modeling. Our method is based on

the evolution of the relativistic MHD equation set together with two additional

equations, describing the evolution of the maximum particles energy and the

downstream particle number density.

Co-‐authors: L.Del Zanna, E. Amato, N. Bucciantini

21. L. Lipatova

The spectrum of the relativistic radiation of electric charges and dipoles in their free fall

into a black hole

The free fall of the electric charges and dipoles, radial and freely falling into the black

hole event horizon was considered. Inverse effect of electromagnetic fields on the black

hole is neglected. Dipole was considered as a point particle, so the deformation

associated with exposureit tidal forces are neglected. According to the theorem, "the

lack of hair" for black holes, multipole magnetic fields must be fully emitted by multipole

fall into a black hole. The spectrum of electromagnetic radiation power for these

multipoles(monopole and dipole) was found. Differences were found in the spectra for

different orientations of the incident dipole. A general method for finding the radiated

electromagnetic multipole fields for the free-‐falling into a black hole multipoles

(including forhigher order multipoles -‐ quadrupoles, etc.). The electromagnetic

spectrum can be compared with observational data from stellar mass black holes and

smaller.

Co-‐authors: I.D. Novikov, A.A. Shatskiy

22. M. Weidl

Cosmic-‐Ray Transport in Turbulent Magnetic Fields

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N/A

23. D. Donevski

Probing Star Formation Rate/ Core Collapse Supernovae Rate

According to some notable works, efficiency of optical luminous Core Collapse

Supernovae is higher than the Supernova Rate (SNR) measured by actual supernovae

surveys. Normalization discrepancy revealed as a factor of 2, and this is so-‐called

“Supernovae Rate Problem” – measured rate is about factor smaller than that predicted

from star formation rate. The main goal of this work is to connect that discrepancy

factor with evolution of stellar component of lithium, because lithium is a tracer of star

formation cosmic rays.

24. H. Lee

CR-‐hydro-‐NEI Models of Particle Acceleration and Broadband Emission at TeV-‐bright Non-thermal

SNRs

We have investigated particle acceleration and the origin of the multi-‐wavelength

emission at young shell-‐type SNRs, in particular those that are bright in the TeV band

and non-‐thermal dominated in X-‐ray. We will present results for two illustrative

examples here, including SNR RX J1713.7-‐3946 and Vela Jr. Using the self-‐consistent

modeling platform provided by a generalized CR-‐hydro-‐NEI code developed by us, we

have constrained possible broadband models under the assistance of the rich library of

observation data. We have found strong evidences that the luminous gamma-‐ray

emission are most convincingly explained by a leptonic-‐dominated origin (i.e. inverse-‐

Compton scatterings by CR electrons) rather than by a hadronic origin related to CR ions,

unless the SNR shock is running into a highly inhomogeneous medium with dense gas

cores such as a clumpy molecular cloud. The thermal X-‐ray lines, whose spectra can be

self-‐consistently calculated by the CR-‐hydro-‐NEI code, turn out to be especially

important in disentangling the origin of the high-‐energy emission. We will discuss

implications of our models on future observations of non-‐thermal SNRs by the next-generation

telescopes including Astro-‐H and CTA.

Co-‐authors: Donald C. Ellison, Patrick Slane, Shigehiro Nagataki and Daniel J. Patnaude

25. E. Fedorova

Variability of the X-‐ray spectral shape of NGC 4945: what do we see with INTEGRAL

Here we present the result of our treatment of the INTEGRAL of the six-‐years

monitoring of the Compton-‐thick Seyfert 2 galaxy NGC 4945. Additionally the data of

two XMM-‐Newton bservations were analyzed. The main results of our investigation is a

disclosure of the variability of both the spectral shape and total flux level in 3-‐200 keV

energy range. Within the spectral model including the Compton reflection, neutral

absorbtion and an exponential cut-‐off at high energies, which is the best-‐fit in our

consideration, both the high-‐energy cut-‐off and the photon index are varying with time.

We stress out that the periods with the cut-‐off value significantly lower 100 keV occur in

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

contradiction to the spin paradigm. We also compare NGC 4945 with several other

active galaxies contradicting to the spin-‐paradigm prescriptions (i.e. that for the RL

objects the X-‐ray spectrum have to be steeper than for RQ ones, and have the

exponential cut-‐off below 100 keV), which were reported earlier. To unveil the nature of

such variations we need to trace out the link between the X-‐ray spectral shape and the

radio and optical properties of these objects, thus the necessity of further simultaneous

monitoring of them in radio/optical/X-‐ray wavebands is stressed out.

Co-‐authors: prof. Zhdanov V.I.

26. E. Antolini

Long-‐Term Monitoring of PKS 0537-‐441 with Fermi-‐LAT and multiwavelength

observations

We report on multiwavelength observations of the blazar PKS

0537−441(z=0.896)obtained from microwaves through γ rays by SMA, REM, ATOM,

Swift and Fermi mostly during 2008 August–2010 April. Strong variability has been

observed in γ rays, with two major flaring episodes(2009 July and 2010 March) and a

harder-‐when-‐brighter behaviour, quitecommon for flat spectrum radio quasars and low-synchrotron-‐peaked

BL Lacs,in 2010 March. The spectral energy distribution (SED)of

the source cannot be modelled by a simple synchrotron self-‐Compton model, as opposed

to many BL Lacs, but the addition of an external Compton component of seed photons

from a dust torus is needed. The 230 GHz light curve showed an increase simultaneous

with the γ-‐ray one, indicating co-‐spatiality of the mm and γ-‐ray emission region likely at

large distance from the central engine. The low, average, and high activity SED of the

source could be fit changing only the electron distribution parameters, but two breaks in

the electron distribution are necessary. The ensuing extra spectral break, located at NIR-optical

frequencies, together with that in γ rays seem to indicate a common origin, most

likely due to an intrinsic feature in the underlying electron distribution. An overall

correlation between the γ-‐ray band with the R-‐band and K-‐band has been observed with

no significant time lag. On the other hand, when inspecting the light curves on short time

scales some differences are evident. In particular, flaring activity has been detected in

NIR and optical bands with no evident γ-‐ray counterparts in 2009 September and

November. Moderate variability has been observed in X-‐rays with no correlation

between flux and photon index. An increase of the detected X-‐ray flux with no

counterpart at the other wavelengths has been observed in 2008 October, suggesting

once more a complex correlation between the emission at different energy bands.

Co-‐authors: G. Tosti, F. D'ammando, J. Finke, S. Ciprini

27. M. Burgess

Physical Fitting of GRB Spectra

The spectra of gamma-‐ray bursts have historically been fit by the empirical Band

function, a smoothly broken power-‐law, and physical insight into the radiation

mechanisms is inferred from the Band function's spectral parameters. However,

degeneracies in model predictions for Band function parameters makes it difficult to

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

uniquely identify the radiation mechanisms in GRBs making it impossible to rule out

incorrect models. Burgess et al. 2011 showed that direct fitting of a physical synchrotron

model to GRB spectral data is possible which eliminates the need for the Band function.

Here we show that extending this work to other radiation mechanisms on a large sample

of GRBs can help to prune down the forest of GRB models and provide direct insight into

the physical processes occurring during the prompt emission of GRBs

Co-‐authors: Dr. Robert D. Preece

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Schedule

www.issibern.ch/cargese2013

COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

List of Accepted Applicants

Antecki Thorsten ta@tp4.rub.de

Antolini Elisa elisa.antolini@tiscali.it

Araudo Anabella aaraudo@gmail.com

Auchettl Katie kauchettl@cfa.harvard.edu

Babyk Iurii babikyura@gmail.com

Bayirli Arif arif.bayirli@boun.edu.tr

Biteau Jonathan biteau@in2p3.fr

Borwankar Chinmay chinmay@barc.gov.in

Burgess Michael james.m.burgess@nasa.gov

Chang Xiaochuan cxcnearby@126.com

Clavel Maïca maica.clavel@obspm.fr

Cui Yudong yudong.cui@astro.uni-‐tuebingen.de

Dejong Sandra dejong@in2p3.fr

Delgado Laura lauradelgadopardo@gmail.com

Desgardin Thibaut thibaut.desgardin@etud.univ-‐montp2.fr

Dominik Michael mdominik@astrouw.edu.pl

Donevski Darko darko_mohikanac@yahoo.com

Dreyer Frederic frederic.dreyer@gmail.com

Dumas Alexis dumas@clermont.in2p3.fr

Elmellah Ileyk ileyk.elmellah@obspm.fr

Fedorova Elena efedorova@ukr.net

Fouka Mourad m.fouka@craag.dz

Ghezali Karima k.ghezali@gmail.com

Gill Ramandeep rgill@cita.utoronto.ca

Grudzinska Mira mgrudzinska@astrouw.edu.pl

Hervet Olivier olivier.hervet@obspm.fr

Heyl Jeremy heyl@phas.ubc.ca

Jermak Helen h.e.jermak@2012.ljmu.ac.uk

Joshi Jagdish jagdish@rri.res.in

Khalil Mohamad mkhalil@in2p3.fr

Khiali Behrouz bkhiali@usp.br

Kudryashova Nina nina.kudryashova@campus.lmu.de

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COSMIC ACCELERATORS April 29 – May 8 2013 Cargèse, Corse, France

Kundu Esha eshakundu@tifr.res.in

Lecoz Sandra lecoz@lpsc.in2p3.fr

Lee Shiu-‐Hang (Herman) lee@yukawa.kyoto-‐u.ac.jp

Leyder Jean-‐Christophe jc.leyder@nasa.gov

Lipatova Lilia l.n.lipa@gmail.com

Loh Alan alan.loh@obspm.fr

Malacaria Christian malacaria@astro.uni-‐tuebingen.de

Malanchev Konstantin malanchev@physics.msu.ru

Mirabel Felix felix.mirabel@cea.fr

Oceguera Tomas tomas.oceguera@gmail.com

Olmi Barbara barbara@arcetri.astro.it

Onic Dusan donic@matf.bg.ac.rs

Pavlovic Marko marko@math.rs

Peresano Michele peresano.michele@gmail.com

Rani Bindu brani@mpifr-‐bonn.mpg.de

Rodriguez Isabel mirb@st-‐andrews.ac.uk

Romoli Carlo romolic@cp.dias.ie

Rosen Anna rosen@ucolick.org

Rueda Jesus jesus.rueda@uv.es

Sadoyan Abel Avetis asadoyan@ysu.am

Saeedi Sara saeedi@astro.uni-‐tuebingen.de

Sajan Kumar sajan@udel.edu

Schanne Stephane schanne@cea.fr

Siemieniec Grazyna grazyna@oa.uj.edu.pl

Sun Shangyu shangyu.sun.khh@googlemail.com

Supsar Markus markus.supsar@tp4.rub.de

Tchernin Celine Celine.Tchernin@unige.ch

Ukwatta Tilan tilan.ukwatta@gmail.com

Vaupre Solenn solenn.vaupre@obs.ujf-‐grenoble.fr

Vila Gabriela gvila@fcaglp.unlp.edu.ar

Vovk Ievgen Ievgen.Vovk@unige.ch

Vuillaume Thomas thomas.vuillaume@obs.ujf-‐grenoble.fr

Weidl Martin martin.weidl@ipp.mpg.de

Yuan Yajie yuanyj@stanford.edu

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Zimmer Stephan zimmer@fysik.su.se

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