| Name: | Rupesh Behera |
| Affiliation: | Indian Institute of Astrophysics |
| Conference ID : | ASI2024_680 |
| Title : | A comparative study of eastern and southern regions of Cygnus loop in x-ray. |
| Authors : | Rupesh Behera1, F. Sutaria1 |
| Authors Affiliation: | 1 Rupesh Behera, F. Sutaria Affiliation (Indian Institute of Astrophysics, Bengalore -560034, India) |
| Mode of Presentation: | Poster |
| Abstract Category : | Stars, Interstellar Medium, and Astrochemistry in Milky Way |
| Abstract : | The supernova remnant (SNR) consists of enriched material ejected in the supernova explosion itself, which, depending on the age of the remnant, is mixed, to extent, with the interstellar material swept up by the passage of the shock wave from the exploded star. SNRs plays an important role in the evolution of a galaxy. All the heavy elements found in the galaxy are produced and distributed by SNRs. We present here our study on Cygnus loop which is a galactic SNR. The Cygnus loop is nearly spherically symmetrical in x-ray, with the exception of a few breakaway patches in the southern region. The mass of the progenitor star of the Cygnus loop is estimated to be 12-15 Mo , which suggests that the compact object left behind might be a neutron star. However, no compact stellar remnant had been confidently detected despite extensive searches. We examined Astrosat-SXT proprietary data as well as Chandra and XMM-Newton archival data from two different regions of the Cygnus loop. Previous studies on other regions of Cygnus loop show a possible presence of charge exchange(CX) reaction in emitting x-ray lines especially in the lower energy region of the soft x-ray band. We studied the x-ray emissions from the eastern part of the Cygnus loop and upon analysis found an enhancement in the abundance of several elements when fitted with thermal emission models like vvpshock, similar to the previous studies. We propose that the cause of this discrepancy in abundance could be due to the contamination of CX. It is nearly impossible to identify each of the CX emission lines from the thermal ones due to the low resolution of the spectrum. For further detailed analysis, highly resolved x-ray spectra will be required to resolve out the individual lines and get an accurate abundance value. |
