Christine Sutton
(CERN)
21/01/2015, 09:10
Manuela Vecchi
(Universidade de Sao Paulo (BR))
21/01/2015, 11:20
The AMS-02 detector is a general purpose particle physics detector installed on the International Space Station to perform a unique long duration mission of fundamental physics research in space. The detector is operating at an altitude of 400 km, detecting cosmic rays in the GeV to TeV range, before they interact with the Earth atmosphere. The main goals of the experiment include the precise...
Serap Tilav
(Univ. of Delaware)
21/01/2015, 12:00
Andrey Turundaevskiy
(Skobeltsyn Institute of Nuclear Physics, Moscow State University, Moscow, 119991, Russia)
21/01/2015, 12:40
The NUCLEON satellite experiment is designed to investigate directly, above the atmosphere, the energy spectra of cosmic-ray nuclei and the chemical composition (Z=1-30) at energy range 100 GeV - 1000 TeV. The effective geometric factor is more than 0.2 m2sr for nuclei and 0.06 m2sr for electrons. The planned exposition time is more than 5 years.
Prof.
Pasquale Blasi
(Osservatorio Astrofisico di Arcetri)
21/01/2015, 14:30
Gwenael Giacinti
(University of Oxford, Clarendon Laboratory)
21/01/2015, 15:30
Analyses of TeV-PeV cosmic ray (CR) diffusion around their sources usually assume either isotropic diffusion, or anisotropic diffusion due to the regular Galactic magnetic field in the spiral arms of our Galaxy. We show that none of these descriptions is adequate on distances smaller than a few coherence lengths (~ 10 pc) of the turbulent interstellar magnetic field.
As a result, we predict...
Dr
Paolo Desiati
(WIPAC - University of Wisconsin, Madison)
21/01/2015, 16:40
This is a review of the observations of cosmic ray anisotropy in a wide energy range, spanning from sub-TeV to EeV energy range. The observations will be described, addressing the different experimental techniques used at the various energy ranges, and stressing the potential physical mechanism they are able to probe. Proposed scenarios that address the origin of the cosmic ray anisotropy will...
Segev BenZvi
(urn:Google)
21/01/2015, 17:20
The High-Altitude Water Cherenkov Observatory, or HAWC, is an air shower array in central Mexico designed to observe cosmic rays and gamma rays between 100 GeV and 100 TeV. HAWC will be completed in early 2015, but has been collecting data in a partial configuration since mid-2013. With only part of the final array in data acquisition, HAWC has already accumulated a data set of nearly 100...
Julia Tjus
22/01/2015, 09:00
Juan Antonio Aguilar Sanchez
(Unknown)
22/01/2015, 10:00
The IceCube Neutrino Observatory is a kilometer-scale neutrino telescope located at the South Pole underneath the Antarctic ice. In the last years IceCube has provided evidence of a diffuse flux component of high-energy astrophysical neutrinos at the level of 10-8 GeV cm-2 s-1 sr-1 per flavor. The origin of these neutrinos remains, however, unknown. Ongoing analyses are trying to solve this...
Charles Dermer
(Naval Research Laboratory)
22/01/2015, 11:00
Results relevant to the question of Galactic cosmic-ray origin are presented. These include updates on hadronic strong-interaction cross sections for the production of secondary gamma rays, leptons and neutrinos, and the use of these cross sections to reveal cosmic-ray interactions and the cosmic-ray spectra in analyses of Fermi-LAT data on supernova remnants and the diffuse Galactic gamma-ray...
Roland Walter
(University of Geneva)
22/01/2015, 11:40
Eta Carinae is the colliding wind binary with the largest mass loss rate in our Galaxy and the only one in which hard X-ray and gamma-ray emission has been detected. Eta Carinae is therefore a primary candidate to search for particle acceleration. We present preliminary gamma-ray data covering two periastron passages. The source variability can be compared with the results of hydrodynamic...
Dr
Giovanna Pedaletti
(DESY Zeuthen)
22/01/2015, 12:00
The association of very-high energy sources with regions of the sky rich in dust and gas has been noticed in the study of individual very-high energy (VHE; E > 100 GeV) sources. However, the statistical significance of this correlation for the whole population of TeV detections has not been assessed yet. To trace the material content, we make use of the recently released all-sky maps of...
Dr
Stefano Gabici
(Laboratoire APC - AstroParticule et Cosmologie)
22/01/2015, 14:00
Dr
Andrew Taylor
(Dublin Institute for Advanced Studies)
22/01/2015, 14:40
Using different Monte Carlo codes such as Geant 4.10, Pythia 8.18, SIBYLL and QGSJET, as well as compiling published data on $pp$ interactions close to the kinematic threshold, we parametrize the energy spectra and production rates of gamma-rays by simple but quite accurate ($\leq 20 \%$) analytical expressions in a broad range from the kinematic threshold to PeV energies.
Carmelo Evoli
(Hamburg University)
22/01/2015, 15:20
At GeV-TeV energies the propagation of CRs is diffusive. Current models of galactic propagation are based on a simplified approach for which diffusion is constant and isotropic.
In fact, diffusion transport must be described as in-homogenous and anisotropic and experimental data have now reached an accuracy that allows to study such effects.
In my talk, I will present some of the...
Timur Delahaye
(Oskar Klein Centre)
22/01/2015, 15:40
Recent results from the AMS-02 data have confirmed that the cosmic ray positron fraction increases with energy between 10 and 200GeV. This quantity should not exceed 50%, and it is hence expected that it will either converge towards 50% or fall. We study the possibility that future data may show the positron fraction dropping down abruptly to the level expected with only secondary production,...
Martina Cardillo
(INAF - Osservatorio astrofisico di Arcetri)
22/01/2015, 16:00
One of the main open issues about the origin of Galactic CRs is the maximum energy that can be achieved by acceleration in Supernova Remnants.
In a rigidity dependent acceleration mechanism, protons are expected to reach a few PeV and heavier ions correspondingly higher energies.
A recent theory suggests that, in a core-collapse SNR expanding in its pre-supernova wind, magnetic field...
Prof.
Isabelle Grenier
(AIM, Université Paris Diderot & CEA Saclay)
22/01/2015, 16:50
The gamma radiation spawn by cosmic rays along their interstellar journey has received much attention over the years as an efficient means to trace the evolution of the cosmic-ray flux and spectrum on kiloparsec scales across the Milky Way.
The data are interpreted in the framework of an elementary scenario which involves cosmic-ray production by diffusive shock acceleration in supernova...
Dr
Ievgen Vovk
(Max Planck Institute for Physics)
22/01/2015, 17:30
SNRs are commonly believed to be the accelerators of the galactic cosmic rays -- mainly protons -- and are expected to produce $\gamma$-rays through the inelastic proton-proton collisions. Fermi/LAT was expected to detect many of those, but only a dozen is listed in the most up to date Fermi/LAT 2nd Source catalogue. To test whether the observed number of SNRs is in agreement with the...
Dr
Ryan Chaves
(Laboratoire Univers et Particules de Montpellier)
23/01/2015, 09:20
The H.E.S.S. Galactic Plane Survey was an ambitious observational program which spanned a period of over 10 years, finishing just recently in 2013. The rich data set accumulated covers nearly the entire Galactic plane visible from Namibia; has an unprecedented, deep sensitivity; and features an energy coverage and angular resolution which is well suited for the search for sources of Galactic...
Dr
Ignasi Reichardt
(INFN, Padova University)
23/01/2015, 10:00
Massive star-forming regions assemble a large number of young stars with remnants of stellar evolution and a very dense environment. Therefore, particles accelerated in supernova remnants and pulsar wind nebulae encounter optimal conditions for interacting with target material and photon fields, and thus produce gamma-ray emission. However, observations are challenging because multiple...
Petra Huentemeyer
(urn:Google)
23/01/2015, 10:50
The High-Altitude Water Cherenkov (HAWC) TeV Gamma-Ray Observatory located at a site about two hours' drive east of Puebla, Mexico on the Sierra Negra plateau (4100 m a.s.l.) will be inaugurated in March 2015. The array of 250 water Cherenkov detectors can observe large portions of the sky simultaneously and, with an energy range of 100 GeV to 100 TeV, is currently one of the most sensitive...
Prof.
Amanda Weinstein
(Iowa State University, Physics & Astronomy Department)
23/01/2015, 11:30
The Cygnus-X star-forming region ("Cygnus") is the richest star-forming region within 2 kpc of Earth and is home to a wealth of potential cosmic ray accelerators, including supernova remnants, massive star clusters, and pulsar wind nebulae. Over the past five years, discoveries by several gamma-ray observatories sensitive in different energy bands, including the identification by Fermi-LAT of...
Teresa Montaruli
23/01/2015, 12:10
The Cherenkov Telescope Array will be the first open access gamma-ray ground-based observatory. I will describe the project, its physics goals, its potential compared to existing experiments, its current status and the schedule.
Andrii Neronov
(University of Geneva)
23/01/2015, 14:20
Ms
Marta D'Angelo
(Gran Sasso Science Institute - INFN)
Electron-positron pair plasmas are believed to play a role in a wide range of cosmic ray sources, including for example relativistic jets from Active Galactic Nuclei or wind outflows in Pulsar Wind Nebulae. One of the key points to understand cosmic ray acceleration is the generation of turbulent magnetic field near the shock front via plasma instabilities. In this work we investigate the...
Mr
Stanislav Stefanik
(Institute of Particle and Nuclear Physics, Charles University)
We examine temporal evolution of the observed $\gamma$-ray intensity from the direction of the
binary PSR B1259-63 using only numbers of detected very high energetic photons.
Simple and straightforward method is applied to the published data obtained with the
Imaging Atmospheric Cherenkov Technique during campaigns around three periastron passages of
the binary system.
Changes...
