| Issue |
A&A
Volume 505, Number 2, October II 2009
|
|
|---|---|---|
| Page(s) | 641 - 654 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/200809473 | |
| Published online | 28 July 2009 | |
Theory of cosmic ray and γ-ray production in the supernova remnant RX J0852.0-4622*
1
Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy, 31 Lenin Ave., 677980 Yakutsk, Russia e-mail: berezhko@ikfia.ysn.ru
2
Landessternwarte, Königstuhl, 69117 Heidelberg, Germany e-mail: Gerd.Puehlhofer@lsw.uni-heidelberg.de
3
Max-Planck-Institut für Kernphysik, Postfach 103980, 69029 Heidelberg, Germany e-mail: Heinrich.Voelk@mpi-hd.mpg.de
Received:
28
January
2008
Accepted:
23
June
2009
Aims. The properties of the Galactic supernova remnant (SNR) RX J0852.0-4622 are theoretically analysed.
Methods. An explicitly time-dependent, nonlinear kinetic
model of cosmic ray (CR) acceleration in SNRs is used to describe the
properties of SNR RX J0852.0-4622, the accelerated CRs, and the nonthermal emission. The
source is assumed to be at a distance of 
1 kpc in the wind bubble
of a massive progenitor star. An estimate of the thermal X-ray flux in this
configuration is given.
Results. We find that the overall synchrotron spectrum of RX J0852.0-4622 as well as the
filamentary structures in hard X-rays lead to an amplified magnetic field 
G in the SNR interior. This implies that the leptonic very high
energy (VHE) γ-ray emission is suppressed, and that the VHE γ-rays are
hadronically dominated. The energy spectrum of protons produced over the
lifetime of the remnant until now may well reach “knee” energies. The
derived γ-ray morphology is consistent with the HESS measurements. The
amount of energy in energetic particles corresponds to about 35% of the
hydrodynamic explosion energy. A remaining uncertainty concerns the thermal
X-ray flux at 1 keV. A rough estimate, which is possibly not quite
appropriate for the assumed wind bubble configuration, is found to be higher
than the nonthermal flux at this energy.
Conclusions. It is concluded that this SNR expanding into the wind bubble of a massive star in a dense gas environment can be a hadronic γ-ray source that is consistent with all existing multiwavelength constraints, except possibly the thermal X-ray emission.
Key words: ISM: cosmic rays / acceleration of particles / shock waves / supernovae: individual: SNR RX J0852.0-4622 / radiation mechanisms: non-thermal / gamma rays: theory
© ESO, 2009
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