Close, bright and boxy: the superluminous SN 2018hti
Fiore A.; Benetti S.; Nicholl M.; Reguitti A.; Cappellaro E.; Campana S.; Bose S.; Paraskeva E.; Berger E.; Bravo T. M.; Burke J.; Cai Y.-Z.; Chen T.-W.; Chen P.; Ciolfi R.; Dong S.; Gomez S.; Gromadzki M.; Gutiérrez C. P.; Hiramatsu D.; Hosseinzadeh G.; Howell D. A.; Jerkstrand A.; Kankare E.; Kozyreva A.; Maguire K.; McCully C.; Ochner P.; Pellegrino C.; Pignata G.; Post R. S.; Rosa N. E.; Shahbandeh M.; Schuldt S.; Thomas B. P.; Tomasella L.; Vinkó J.; Vogl C.; Wheeler J. C.; Young D. R.
https://urn.fi/URN:NBN:fi-fe2022081154537
Tiivistelmä
SN~2018hti was a very nearby (z=0.0614) superluminous supernova with an exceedingly bright absolute magnitude of -22.2 mag in r-band at maximum. The densely sampled pre-maximum light curves of SN~2018hti show a slow luminosity evolution and constrain the rise time to ~50 rest-frame days. We fitted synthetic light curves to the photometry to infer the physical parameters of the explosion of SN 2018hti for both the magnetar and the CSM-interaction scenarios. We conclude that one of two mechanisms could be powering the luminosity of SN 2018hti; interaction with ~10 Msun of circumstellar material or a magnetar with a magnetic field of B_p~1.3e13 G and initial period of P_spin~1.8 ms. From the nebular spectrum modelling we infer that SN 2018hti likely results from the explosion of a ~40 Msun progenitor star.
Kokoelmat
- Rinnakkaistallenteet [29335]