On the Origin of the Asymmetry of the Ejecta Structure and Explosion of G350.1–0.3

We present X-ray analysis of the ejecta supernova remnant G350.1$-$0.3 observed with Chandra and Suzaku, clarify ejecta's kinematics over a decade obtain new observational clue to understanding origin asymmetric explosion. Two images Observatory taken in 2009 2018 are analyzed several methods, enable us measure velocities plane sky. A maximum velocity is 4640$\pm$290 km s$^{-1}$ (0.218$\pm$0.014 arcsec yr$^{-1}$) eastern region remnant. These findings trigger scrutinize Doppler effects spectra thermal emission, line-of-sight direction estimated be thousand s$^{-1}$. The results confirmed by analyzing Suzaku. Combining proper motions velocities, three-dimensional $\sim$3000-5000 center explosion more stringently constrained finding optimal time reproduce spatial expansion. Our that age SNR at most 655 years, CCO as point source object against strengthen 'hydrodynamical kick' hypothesis on