Статья

Fast evolving pair-instability supernova models: evolution, explosion, light curves

Alexandra KozyrevaAstrophysics group, Keele University, Keele, Staffordshire ST5 5BG, UKMatthew GilmerDepartment of Physics, North Carolina State University, Raleigh, NC 27695-8202, USARaphaël HirschiAstrophysics group, Keele University, Keele, Staffordshire ST5 5BG, UKCarla FröhlichDepartment of Physics, North Carolina State University, Raleigh, NC 27695-8202, USAС. И. БлинниковITEP (Kurchatov Institute), Moscow 117218, RussiaRyan WollaegerCenter for Theoretical Astrophysics/CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87544, USAU. M. NoebauerMax-Planck-Institut fr Astrophysik, Karl-Schwarzschild-Strae 1, D-85748 Garching, GermanyDaniel R. van RossumFlash Center for Computational Science, University of Chicago, Chicago, IL 60637, USAAlexander HegerSchool of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USAWesley EvenCenter for Theoretical Astrophysics/CCS-2, Los Alamos National Laboratory, Los Alamos, NM 87544, USARoni WaldmanRacah Institute of Physics, The Hebrew University, Jerusalem 91904, IsraelAlexey TolstovKavli Institute for the Physics and Mathematics of the Universe (WPI), Tokyo Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, JapanE. ChatzopoulosDepartment of Physics and Astronomy, Louisiana State University, Baton Rouge, LA 70803-4001, USAE. I. SorokinaSternberg Astronomical Institute, M.V. Lomonosov Moscow State University, Moscow 119991, Russia

2016en

ABI

Аннотация

With an increasing number of superluminous supernovae (SLSNe) discovered, the question of their origin remains open and causes heated debates in the supernova community. Currently, there are three proposed mechanisms for SLSNe: (1) pair-instability supernovae (PISNe), (2) magnetar-driven supernovae and (3) models in which the supernova ejecta interacts with a circumstellar material ejected before the explosion. Based on current observations of SLSNe, the PISN origin has been disfavoured for a number of reasons. Many PISN models provide overly broad light curves and too reddened spectra, because of massive ejecta and a high amount of nickel. In the current study, we re-examine PISN properties using progenitor models computed with the GENEC code. We calculate supernova explosions with FLASH and light-curve evolution with the radiation hydrodynamics code STELLA. We find that high-mass models (200 and 250 M ) at relatively high metallicity (Z = 0.001) do not retain hydrogen in the outer layers and produce relatively fast evolving PISNe Type I and might be suitable to explain some SLSNe. We also investigate uncertainties in light-curve modelling due to codes, opacities, the nickel-bubble effect and progenitor structure and composition.

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Идентификаторы

DOI: 10.1093/mnras/stw2562

Цитирования и источники

Цитирований: 2Использованных источников: 0

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