Volume 593, September 2016
|Number of page(s)||10|
|Section||Interstellar and circumstellar matter|
|Published online||31 August 2016|
Modeling the shock-cloud interaction in SN 1006: Unveiling the origin of nonthermal X-ray and γ-ray emission
1 Dipartimento di Fisica &
ChimicaUniversità di Palermo, Piazza
del Parlamento 1, 90134 Palermo, Italy
2 INAF-Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
3 Dpto. de Astrofísica y CC de la Atmósfera, Universidad Complutense de Madrid, 28040 Madrid, Spain
4 Laboratoire AIM, CEA-IRFU/CNRS/Université Paris Diderot, Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France
5 Department of Physics, Faculty of Science & Engineering, Chuo University, 1-13-27 Kasuga, Bunkyo, 112-8551 Tokyo, Japan
6 Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette Cedex, France
7 Department of Physics, Middlebury College, Middlebury, VT 05753, USA
8 Department of Astronomy, University of Michigan, 311 West Hall, 1085 S, University Ave, Ann Arbor, MI 48109-1107, USA
9 Instituto de Astronomía y Física del Espacio (IAFE), UBA-CONICET, CC 67, Suc. 28, 1428 Buenos Aires, Argentina
Accepted: 24 June 2016
Context. The supernova remnant SN 1006 is a source of high-energy particles and its southwestern limb is interacting with a dense ambient cloud, thus is a promising region for γ-ray hadronic emission.
Aims. We aim at describing the physics and the nonthermal emission associated with the shock-cloud interaction to derive the physical parameters of the cloud (poorly constrained by the data analysis), to ascertain the origin of the observed spatial variations in the spectral properties of the X-ray synchrotron emission, and to predict spectral and morphological features of the resulting γ-ray emission.
Methods. We performed 3D magnetohydrodynamic simulations modeling the evolution of SN 1006 and its interaction with the ambient cloud, and explored different model setups. By applying the REMLIGHT code on the model results, we synthesized the synchrotron X-ray emission and compared it with actual observations to constrain the parameters of the model. We also synthesized the leptonic and hadronic γ-ray emission from the models, deriving constraints on the energy content of the hadrons accelerated at the southwestern limb.
Results. We found that the impact of the SN 1006 shock front with a uniform cloud with density 0.5 cm-3 can explain the observed morphology, the azimuthal variations of the cutoff frequency of the X-ray synchrotron emission, and the shock proper motion in the interaction region. Our results show that the current upper limit for the total hadronic energy in the southwestern limb is 2.5 × 1049 erg.
Key words: X-rays: ISM / ISM: supernova remnants / ISM: individual objects: SN 1006 / ISM: clouds / acceleration of particles / magnetohydrodynamics (MHD)
© ESO 2016
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