On the origin of the asymmetry of the ejecta structure and explosion of G350.1−0.3
Links to Fileshttps://arxiv.org/abs/2104.03001
MetadataShow full item record
Type of Work12 pages
journal articles preprints
Citation of Original PublicationTomoya Tsuchioka, Yasunobu Uchiyama, Ryota Higurashi, Hiroyoshi Iwasaki, Shumpei Otsuka, Shinya Yamada and Toshiki Sato, On the origin of the asymmetry of the ejecta structure and explosion of G350.1−0.3, https://arxiv.org/abs/2104.03001
RightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
Attribution 4.0 International
We present X-ray analysis of the ejecta of supernova remnant G350.1−0.3 observed with Chandra and Suzaku, and clarify the ejecta's kinematics over a decade and obtain a new observational clue to understanding the origin of the asymmetric explosion. Two images of Chandra X-ray Observatory taken in 2009 and 2018 are analyzed in several methods, and enable us to measure the velocities in the plane of the sky. A maximum velocity is 4640±290 km s⁻¹ (0.218±0.014 arcsec yr⁻¹) in the eastern region in the remnant. These findings trigger us to scrutinize the Doppler effects in the spectra of the thermal emission, and the velocities in the line-of-sight direction are estimated to be a thousand km s⁻1. The results are confirmed by analyzing the spectra of Suzaku. Combining the proper motions and line-of-sight velocities, the ejecta's three-dimensional velocities are ∼3000-5000 km s⁻¹. The center of the explosion is more stringently constrained by finding the optimal time to reproduce the observed spatial expansion. Our findings that the age of the SNR is estimated at most to be 655 years, and the CCO is observed as a point source object against the SNR strengthen the 'hydrodynamical kick' hypothesis on the origin of the remnant.
The following license files are associated with this item:
- Creative Commons