Conveners
Session 3: Cosmic rays(1poster)
- Qiang Yuan (Purple Mountain Observatory)
Session 3: Cosmic rays
- Carmelo Evoli (SNS, Pisa, Italy)
Session 3: Cosmic rays
- Hao Zhou (Shanghai Jiao Tong University)
Description
posters shown at break time
Chuan YUE
(Purple Mountain Observatory)
10/26/21, 3:00 PM
oral
The DArk Matter Particle Explorer (DAMPE) is a space-based mission designed as a high energy particle detector for measuring cosmic-rays and gamma-rays in space. It was successfully launched on December 17, 2015, and since then has been in stable data taking for more than five and a half years. The large geometric factor and thick calorimeter enables DAMPE to have very good potential to...
Dimitrios Kyratzis
(Gran Sasso Science Institute (GSSI) and INFN-LNGS)
10/26/21, 3:20 PM
oral
The Dark Matter Particle Explorer (DAMPE), is a space–borne detector designed for precise galactic Cosmic Ray (CR) studies in a wide energy range (up to hundreds of TeV), along with detailed measurements of high–energy gamma–rays and indirect searches of Dark Matter (DM) annihilation/decay to detectable particles. The satellite was successfully launched into a sun–synchronous orbit at 500 km,...
Michael Korsmeier
(O)
10/26/21, 4:00 PM
oral
Space-borne experiments like AMS-02 determine cosmic-ray spectra with unprecedented precision. This allows for more elaborate and better examinations of cosmic-ray propagation in our Galaxy. However, the analysis of this increasingly precise cosmic-ray data requires also a more careful assessment of systematic uncertainties. I will present the results from the analysis of comic-ray...
Vo Hong Minh Phan
(TTK, RWTH Aachen University)
10/26/21, 4:20 PM
poster
Supernova remnants interacting with molecular clouds are ideal laboratories to study the acceleration of particles at shock waves and their transport and interactions in the surrounding interstellar medium. In this paper, we focus on the supernova remnant W28, which over the years has been observed in all energy domains from radio waves to very-high-energy gamma rays. The bright gamma-ray...
Dr
Siming Liu
(Purple Mountain Observatory)
10/26/21, 4:40 PM
oral
In this talk, I will review our recent multiwavelength study of a sample of gamma-ray supernova remnants (SNRs), which can be used to constrain evolution of high energy particles in SNRs. Our results suggest that shocks of SNRs may not be efficient PeVatrons. However, they can readily accelerate particles to about 100 TeV. In particular, shocks of the supernova that gave rise to the Geminga...
Dr
Pierre Cristofari
(Observatoire de Paris)
10/26/21, 5:00 PM
oral
The search for pevatrons (objects capable of accelerating partilces up to 10$^{15}$ eV) has become one of the key targets of the high--energy gamma--ray community.
These objects are of crucial importance in the context of the origin of cosmic rays (CRs), since the sources of Galactic CRs are expected to
be able to accelerate particles up to PeV energies, at least at some stage of their...
Dr
Vo Hong Minh Phan
(TTK, RWTH Aachen University)
10/26/21, 5:20 PM
oral
Data from the Voyager probes have provided us with the first measurement of cosmic ray intensities at MeV energies, an energy range that had previously not been explored. Simple extrapolations of models that fit data at GeV energies, e.g., from AMS-02, however, fail to reproduce the Voyager data in that the predicted intensities are too high. Oftentimes, this discrepancy is addressed by adding...
Dr
Naveen Kumar
(Max-Planck Institute for Nuclear Physics)
10/27/21, 3:00 PM
oral
Electron and ion acceleration at a non-relativistic collisionless shocks is studied by employing large scale one-dimensional particle-in-cell (PIC) simulations in the de-Hoffmann and Teller (dHT) frame of reference. We demonstrate that diffusive shock acceleration of both electrons and ions occurs in quasi-perpendicular shock configurations at large Alfvén Mach numbers. We also identify the...
Robert Brose
(Dublin Institute of Advanced Studies)
10/27/21, 3:20 PM
oral
Supernova remnants are known to accelerate cosmic rays (CRs) on account of their non-thermal emission of radio waves, X-rays, and gamma rays. However, the ability to accelerate CRs up to PeV-energies has yet to be demonstrated. The presence of cut-offs in the gamma-ray spectra of several young SNRs led to the idea that PeV energies might only be achieved during the very initial stages of a...
Ms
Samata Das
(DESY, Institute of Physics and Astronomy, University of Potsdam, Germany)
10/27/21, 3:40 PM
oral
**Context.** Supernova Remnants (SNRs) are considered as the primary sources of galactic cosmic rays (CRs), accelerated by diffusive shock acceleration (DSA) mechanism at SNR shocks. The core-collapse SNRs expand in the complex ambient environment, inside wind-blown bubbles created by the mass-loss of massive stars during their different evolutionary stages. Therefore, the evolution of...
Ottavio Fornieri
(The Gran Sasso Science Institute)
10/27/21, 4:40 PM
oral
We present the phenomenological implications of the micro-physics of CR diffusion as resulting from particle scattering onto the three modes in which \textit{Magneto-Hydro-Dynamics} (MHD) cascades are decomposed. We calculate the diffusion coefficients from first principles based on reasonable choices of the physical quantities characterizing the different environments of our Galaxy, namely...
Benedikt Schroer
(G)
10/27/21, 5:00 PM
oral
In the typical picture of cosmic ray transport in the region around their sources cosmic rays escape along the local magnetic field lines. We investigate this phenomenon using 2D and 3D hybrid particle-in-cell simulations.
The escaping cosmic rays excite resonant and non-resonant streaming instabilities resulting in enhanced particle scattering. This leads to a large pressure gradient that...
Marco Kuhlen
(TTK Institute, RWTH-Aachen)
10/29/21, 3:00 PM
oral
In the standard picture of cosmic ray transport the propagation of charged cosmic rays through turbulent magnetic fields is described as a random walk with cosmic rays scattering on magnetic field turbulence. This is in good agreement with the highly isotropic arrival directions as this diffusion process effectively isotropizes the cosmic ray distribution. However, high-statistics...
Gwenael Giacinti
(MPIK Heidelberg)
10/29/21, 3:20 PM
oral
We calculate the shape of the TeV-PeV cosmic-ray anisotropy (CRA) in 3D Kolmogorov turbulence. We present the first numerical calculations of the CRA down to TeV energies, using realistic values for the coherence length of the interstellar turbulence. At these low energies, the large-scale CRA aligns with the direction of local magnetic field lines around the observer. In this type of...
Julien Dörner
(Ruhr-University Bochum)
10/29/21, 3:40 PM
oral
The propagation of cosmic rays can be described as a diffusive motion in most galactic environments. The Milky Way and its cosmic-ray distribution have been studied in detail by the measurement of high-energy gamma-rays with Fermi. A gradient in the cosmic-ray density and spectral energy behavior has been measured indirectly this way and is in need of explanation.
In this talk we use recent...
Dr
Juan Wu
(China University of Geosciences)
10/29/21, 4:40 PM
oral
Thanks to the precise cosmic ray data measured by recent
space experiments, we are able to investigate the cosmic ray acceleration and propagation mod-
els more comprehensively and reliably. In this work, we combine the secondary-to-primary ratio
and the primary spectra measured by PAMELA, AMS02, ACE-CRIS and Voyager-1 to constrain
the cosmic ray source and transport parameters. The study...
Pedro De la Torre Luque
(Stockholms universitet)
10/29/21, 5:00 PM
oral
he propagation of Galactic cosmic rays (CRs) is commonly studied as a diffusive movement which can be evaluated from the spectra of secondary CRs. While the accuracy of current CR data allows us to precisely test our propagation models, the precision of cross sections data for the production of secondary CRs is very poor (>20%), considerably limiting these tests.
In this talk we explore the...
