The supernova remnant SN 1006 as a Galactic particle accelerator

Roberta Giuffrida, Marco Miceli (), Damiano Caprioli, Anne Decourchelle, Jacco Vink, Salvatore Orlando, Fabrizio Bocchino, Emanuele Greco and Giovanni Peres
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Roberta Giuffrida: Università degli Studi di Palermo, Dipartimento di Fisica e Chimica E. Segrè
Marco Miceli: Università degli Studi di Palermo, Dipartimento di Fisica e Chimica E. Segrè
Damiano Caprioli: The University of Chicago
Anne Decourchelle: Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM
Jacco Vink: Anton Pannekoek Institute, GRAPPA, University of Amsterdam
Salvatore Orlando: INAF-Osservatorio Astronomico di Palermo
Fabrizio Bocchino: INAF-Osservatorio Astronomico di Palermo
Emanuele Greco: INAF-Osservatorio Astronomico di Palermo
Giovanni Peres: Università degli Studi di Palermo, Dipartimento di Fisica e Chimica E. Segrè

Nature Communications, 2022, vol. 13, issue 1, 1-11

Abstract: Abstract The origin of cosmic rays is a pivotal open issue of high-energy astrophysics. Supernova remnants are strong candidates to be the Galactic factory of cosmic rays, their blast waves being powerful particle accelerators. However, supernova remnants can power the observed flux of cosmic rays only if they transfer a significant fraction of their kinetic energy to the accelerated particles, but conclusive evidence for such efficient acceleration is still lacking. In this scenario, the shock energy channeled to cosmic rays should induce a higher post-shock density than that predicted by standard shock conditions. Here we show this effect, and probe its dependence on the orientation of the ambient magnetic field, by analyzing deep X-ray observations of the Galactic remnant of SN 1006. By comparing our results with state-of-the-art models, we conclude that SN 1006 is an efficient source of cosmic rays and obtain an observational support for the quasi-parallel acceleration mechanism.

Date: 2022
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DOI: 10.1038/s41467-022-32781-4

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