Science-advisor
REGISTER info/FAQ
Login
username
password
     
forgot password?
register here
 
Research articles
  search articles
  reviews guidelines
  reviews
  articles index
My Pages
my alerts
  my messages
  my reviews
  my favorites
 
 
Stat
Members: 3643
Articles: 2'488'730
Articles rated: 2609

29 March 2024
 
  » arxiv » 2007.14348

 Article overview


SN 2018zd: An Unusual Stellar Explosion as Part of the Diverse Type II Supernova Landscape
Jujia Zhang ; Xiaofeng Wang ; Jozsef Vinko ; Qian Zhai ; Tianmeng Zhang ; Alexei V. Filippenko ; Thomas G. Brink ; WeiKang Zheng ; Lukasz Wyrzykowski ; Przemyslaw Mikolajczyk ; Fang Huang ; Liming Rui ; Jun Mo ; Hanna Sai ; Xinhan Zhang ; Huijuan Wang ; James M. DerKacy ; Eddie Baron ; K. Sarneczky ; A. Bodi ; G. Csornyei ; O. Hanyecz ; B. Ignacz ; Cs. Kalup ; L. Kriskovics ; R. Konyves-Toth ; A. Ordasi ; A. Pal ; A. Sodor ; R. Szakats ; K. Vida ; G. Zsidi ;
Date 28 Jul 2020
AbstractWe present extensive observations of SN 2018zd covering the first $sim450$,d after the explosion. This SN shows a possible shock-breakout signal $sim3.6$,hr after the explosion in the unfiltered light curve, and prominent flash-ionisation spectral features within the first week. The unusual photospheric temperature rise (rapidly from $sim 12,000$,K to above 18,000,K) within the earliest few days suggests that the ejecta were continuously heated. Both the significant temperature rise and the flash spectral features can be explained with the interaction of the SN ejecta with the massive stellar wind ($0.18^{+0.05}_{-0.10}, m M_{odot}$), which accounts for the luminous peak ($L_{ m max} = [1.36pm 0.63] imes 10^{43}, m erg,s^{-1}$) of SN 2018zd. The luminous peak and low expansion velocity ($v approx 3300$ km s$^{-1}$) make SN 2018zd to be like a member of the LLEV (luminous SNe II with low expansion velocities) events originated due to circumstellar interaction. The relatively fast post-peak decline allows a classification of SN 2018zd as a transition event morphologically linking SNe~IIP and SNe~IIL. In the radioactive-decay phase, SN 2018zd experienced a significant flux drop and behaved more like a low-luminosity SN~IIP both spectroscopically and photometrically. This contrast indicates that circumstellar interaction plays a vital role in modifying the observed light curves of SNe~II. Comparing nebular-phase spectra with model predictions suggests that SN 2018zd arose from a star of $sim 12, m M_{odot}$. Given the relatively small amount of $^{56}$Ni ($0.013 - 0.035 m M_{odot}$), the massive stellar wind, and the faint X-ray radiation, the progenitor of SN 2018zd could be a massive asymptotic giant branch star which collapsed owing to electron capture.
Source arXiv, 2007.14348
Services Forum | Review | PDF | Favorites   
 
Visitor rating: did you like this article? no 1   2   3   4   5   yes

No review found.
 Did you like this article?

This article or document is ...
important:
of broad interest:
readable:
new:
correct:
Global appreciation:

  Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.

browser claudebot






ScienXe.org
» my Online CV
» Free


News, job offers and information for researchers and scientists:
home  |  contact  |  terms of use  |  sitemap
Copyright © 2005-2024 - Scimetrica