The metamorphosis of the Type Ib SN 2019yvr: late-time interaction
arxiv(2024)
摘要
We present observational evidence of late-time interaction between the ejecta
of the hydrogen-poor Type Ib supernova (SN) 2019yvr and hydrogen-rich
circumstellar material (CSM), similar to the Type Ib SN 2014C. A narrow
Hα emission line appears simultaneously with a break in the light-curve
decline rate at around 80-100 d after explosion. From the interaction delay and
the ejecta velocity, under the assumption that the CSM is detached from the
progenitor, we estimate the CSM inner radius to be located at 6.5-9.1 ×
10^15 cm. The Hα emission line persists throughout the nebular phase
at least up to +420 d post-explosion, with a full width at half maximum of
2000 km/s. Assuming a steady mass-loss, the estimated mass-loss rate from the
luminosity of the Hα line is 3-7 × 10^-5 M_⊙yr^-1. From
hydrodynamical modelling and analysis of the nebular spectra, we find a
progenitor He-core mass of 3-4 M_⊙, which would imply an initial mass of
13-15 M_⊙. Our result supports the case of a relatively low-mass
progenitor possibly in a binary system as opposed to a higher mass single star
undergoing a luminous blue variable phase.
更多查看译文
AI 理解论文
溯源树
样例
生成溯源树,研究论文发展脉络
Chat Paper
正在生成论文摘要