DS10 - Défi des autres savoirs

PeV Cosmic Rays – PECORA

Extreme particle accelerators in the Galaxy

The goal of this project is to identify the sources of PeV cosmic rays by means of multi-messenger (X-rays, gamma rays, and neutrinos) observations by current and forthcoming leading facilities.

PECORA: PeV Cosmic Rays

More than one century after their discovery, the origin of cosmic rays is still a crucial issue in high energy astrophysics. The chemical compositon of cosmic rays is dominated by protons below a partcle energy of ~1 PeV, while heavier nuclei become important above it. This, together with the evidence that the transiton between galactic and extragalactic cosmic rays takes place at particle energies largely exceeding the PeV, implies that the sources of galactic cosmic rays must be proton PeVatrons. The goal of this project is to identify the sources of PeV cosmic rays by means of multi-messenger (X-rays, gamma rays, and neutrinos) observations by current and future leading facilites.

The project is composed by several Working Packages, and for this reason a number of different methodologies are being used. These span from theoretical calculations to data analysis, to phenomenological approaches.

Several results have already been obtained in various Working Packages, In particular, thanks to X-ray observations of the galactic centre region it was possible to characterise in greater detail the nature of the outflow of matter originating at the Galactic centre. A chimney has been identified, connecting the region immediately surrounding the black hole with the gigantic Fermi Bubbles. This result has been published on Nature.

The project is proceeding as planned, and we expect to deliver a number of results over the next months. In particular, results based on the analysis of HESS and Fermi data on supernova remnants and on potential Galactic PeVatrons.

8 refereed papers published.

More than one century after their discovery, the origin of cosmic rays is still a crucial issue in high energy astrophysics. The chemical composition of cosmic rays is dominated by protons below a particle energy of ~1 PeV, while heavier nuclei become important above it. This, together with the evidence that the transition between galactic and extragalactic cosmic rays takes place at particle energies largely exceeding the PeV, implies that the sources of galactic cosmic rays must be proton PeVatrons. The goal of this project is to identify the sources of PeV cosmic rays by means of multi-messenger (X-rays, gamma rays, and neutrinos) observations by current and future leading facilities.

Project coordination

Stefano Gabici (Astroparticule et Cosmologie)

The author of this summary is the project coordinator, who is responsible for the content of this summary. The ANR declines any responsibility as for its contents.

Partner

IRAP Institut de Recherche en Astrophysique et Planétologie
Centre de Sciences Nucléaires et de Sciences de la Matière
CENBG Centre d'études nucléaires de Bordeaux Gradignan
AIM Astrophysique, Interpretation - Modélisation, Paris-Saclay
Astroparticule et Cosmologie

Help of the ANR 495,467 euros
Beginning and duration of the scientific project: December 2017 - 48 Months

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