A unified picture for three different cosmic-ray observables.

Discussion timeslot (ZOOM-Meeting): 19. July 2021 - 18:00
ZOOM-Meeting URL: https://desy.zoom.us/j/91896950007
ZOOM-Meeting ID: 91896950007
ZOOM-Meeting Passcode: ICRC2021
Corresponding Session: https://icrc2021-venue.desy.de/channel/18-Cosmic-Ray-Secondary-nuclei-observations-and-impact-on-theories-CRD/71
Live-Stream URL: https://icrc2021-venue.desy.de/livestream/Discussion-06/7

Abstract:
'We present here a unified scenario that connects together three peculiar spectral features recently reported in the spectra of charged cosmic rays (CRs).rn The spectral hardening measured by AMS-02 in the hadronic spectra above $sim 250 , mathrm{GeV}$ is here interpreted as a diffusion imprint, and modeled by means of a transport coefficient that smoothly hardens with rigidity. rn We implement such propagation framework to solve the transport equation with the {tt DRAGON2} numerical code in order to determine the large-scale contribution to the CR fluxes. rn On top of this solution we explore the hypothesis of a nearby, hidden Supernova Remnant (SNR) to be responsible for the high-energy (above $sim 100 , mathrm{GeV}$) all-lepton flux, in particular for the spectral break consistently measured by all the space-borne and ground-based detectors around $1 , mathrm{TeV}$. We compute such contribution analytically adopting the same propagation setup implemented for the large-scale background.rn Simultaneously, we find the signature of the same source in the peculiar textit{bump} structure observed by the DAMPE Collaboration in the proton spectrum, consisting of a strong hardening at $sim 500 , mathrm{GeV}$ and a softening at $13 , mathrm{TeV}$. rn We validate our hypothesis with the CR dipole-anisotropy (DA) amplitude and phase. In particular, we interpret the high-energy data (above $10 , mathrm{TeV}$) pointing towards the Galactic Center as the convolution of the directional fluxes of the large-scale-background sources, whereas the DA amplitude below that energy is compatible with the predictions of our model and is therefore considered as a signature of the nearby SNR that we invoke.'

Authors: Ottavio Fornieri | Daniele Gaggero | Daniel Guberman | Loann Brahimi | Pedro De la Torre Luque | Alexandre Marcowith
Indico-ID: 1225
Proceeding URL: https://pos.sissa.it/395/173