Abstract
Modeling thermal X-ray emission from supernova remnant interacting with the CSM
Ekaterina Makarenko, Stefanie Walch
1. Institute of Physics, University of Cologne
RCW 103 is a young (around 2000 years) Galactic supernova remnant (SNR) that has begun interacting with the surrounding circumstellar medium (CSM) and nearby molecular cloud. It has been observed in the X-ray, optical, IR, and radio bands. Despite the SNR having a non-uniform density distribution at the site of the explosion, the X-ray morphology is nearly circular. In this work, we model the X-ray emission from RCW 103 using hydrodynamical simulations. Our model is the first implementation of radiative cooling emission from an SNR treated self-consistently on-the-fly in the ISM using the FLASH code. We calculate the emission and absorption using a backward ray tracing scheme, and each cell within the SNR is treated as a source of radiation. We start with the turbulent interstellar medium and form an HII region around a massive star (20 solar masses) with wind and ionising radiation feedback. At the end of the massive star’s life, we explode the supernova (type II) and follow the radiative cooling emission in several X-ray energy bands (user-defined in the range from 0.1 to 8+keV). We can see how the shock wave evolves, starting to interact with the CSM material. We also apply significant absorption, which varies across the RCW 103 SNR and is stronger in the north and west. As a result, we created synthetic maps of the simulated SNR to reveal the origin and evolution of the circular diffuse X-ray emission.