2009/03/19 by M. Miceli, F. Bocchino, D. Iakubovskyi +6 · 62 citations
Physics and Astronomy · #Anisotropy #Astrophysics and Cosmic Phenomena #Cosmic ray #Ejecta #Gamma-ray bursts and supernovae #Interstellar medium #Particle acceleration #Shock (circulatory) #Solar and Space Plasma Dynamics #Spectral line #Supernova #Supernova remnant #Thermal #astro-ph.HE
paper · pdf · doi:10.1051/0004-6361/200811505
published in Astronomy and Astrophysics 501(1), 239-249 (EDP Sciences) · Accepted for publication in A&A. For the version of the paper with high resolution images, please see http://www.astropa.unipa.it/Library/preprint.html
arxiv created 2009/03/19 · openalex publication_date 2009/04/29 · arxiv updated 2015/05/13 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
<i>Context. <i/>Efficient particle acceleration can modify the structure of supernova remnants. We present the results of a combined analysis of the <i>XMM-Newton<i/> EPIC archive observations of SN 1006.<i>Aims. <i/>We attempt to describe the spatial distribution of the physical and chemical properties of the X-ray emitting plasma at the shock front. We investigate the contribution of thermal and non-thermal emission to the X-ray spectrum at the rim of the remnant to study how the acceleration processes affect the X-ray emitting plasma.<i>Methods. <i/>We perform a spatially resolved spectral analysis of a set of regions covering the entire rim of the shell and we apply our results in producing a count-rate image of the “pure” thermal emission of SN 1006 in the 0.5-0.8 keV energy band (subtracting the non-thermal contribution). This image differs significantly from the total image in the same band, especially close to the bright limbs.<i>Results. <i/>We find that thermal X-ray emission can be associated with the ejecta and study the azimuthal variation in the physical and chemical properties of the ejecta by identifying anisotropies in the temperature and chemical composition. By employing our thermal image, we trace the position of the contact discontinuity over the entire shell and compare it with that expected from 3D MHD models of SNRs with an unmodified shock.<i>Conclusions. <i/>We conclude that the shock is modified everywhere in the rim and that the aspect angle between the interstellar magnetic field and the line of sight is significantly lower than .