The supernova remnant SN 1006

3D ModelNoAI

Structure of SN 1006, the remnant of a type Ia supernova (SN) observed between April 30 and May 1, 1006 in the constellation Lupus. The blast wave from the SN (outer sphere) propagates outward through the interstellar medium (ISM) and a reverse shock (inner sphere) propagates inward through the stellar debris (ejecta). Dust forms in the still unshocked ejecta with temperatures of a few degrees. The material in the mixing region between the two shocks is very hot (tens of millions of degrees) and subject to hydrodynamic instability that develops at the interface between shocked ejecta and shocked ISM. The SNR interacts with interstellar clouds (for instance, on the right); cosmic rays are accelerated at the shock fronts (arrows and yellow regions in the forward shock), producing synchrotron emission.

MHD simulation performed with the FLASH code.

Reference: Orlando et al. 2012, ApJ 749, id. 156.

Credits: INAF/OAPA; SN1006 image by NASA/Chandra.