SN 2018hna: Adding a piece to the puzzles of the explosion of blue supergiants
| Autor: | Danfeng Xiang, Xiaofeng Wang, Xinghan Zhang, Hanna Sai, Jujia Zhang, Thomas G Brink, Alexei V Filippenko, Jun Mo, Tianmeng Zhang, Zhihao Chen, Luc Dessart, Zhitong Li, Shengyu Yan, Sergei I Blinnikov, Liming Rui, E Baron, J M DerKacy |
|---|---|
| Rok vydání: | 2023 |
| Předmět: | |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 520:2965-2982 |
| ISSN: | 1365-2966 0035-8711 |
| Popis: | We present extensive optical/ultraviolet observations and modelling analysis for the nearby SN 1987A-like peculiar Type II supernova (SN) 2018hna. Both photometry and spectroscopy covered phases extending to $>$500 days after the explosion, making it one of the best-observed SN II of this subtype. SN 2018hna is obviously bluer than SN 1987A during the photospheric phase, suggesting higher photospheric temperature, which may account for weaker BaII $\mathrm{\lambda}$6142 lines in its spectra. Analysis of early-time temperature evolution suggests a radius of $\sim$45 $\mathrm{R_{\odot}}$ for the progenitor of SN 2018hna, consistent with a blue supergiant (BSG). By fitting the bolometric light curve with hydrodynamical models, we find that SN 2018hna has an ejecta mass of $\sim$(13.7--17.7) $\mathrm{M_{\odot}}$, a kinetic energy of $\sim$ (1.0--1.2) $\times 10^{51}$ erg, and a $^{56}$Ni mass of about 0.05 $\mathrm{M_{\odot}}$. Moreover, based on standard stellar evolution and the oxygen mass (0.44--0.73 $\mathrm{M_{\odot}}$) deduced from nebular [OI] lines, the progenitor of SN 2018hna is expected to have an initial main-sequence mass $ Comment: 18 pages; accepted for publication in MNRAS |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|