Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1208.1214)
· References in the article
· Citations to the Article (8) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Superluminous supernovae: 56Ni power versus magnetar radiation
Authors:
Dessart, Luc; Hillier, D. John; Waldman, Roni; Livne, Eli; Blondin, Stéphane
Affiliation:
AA(Aix Marseille Université, CNRS, LAM (Laboratoire d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, France; TAPIR, Mail code 350-17, California Institute of Technology, Pasadena, CA 91125, USA), AB(Department of Physics and Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA 15260, USA), AC(Racah Institute of Physics, The Hebrew University, Jerusalem 91904, Israel), AD(Racah Institute of Physics, The Hebrew University, Jerusalem 91904, Israel), AE(Centre de Physique des Particules de Marseille, Université Aix-Marseille, CNRS/IN2P3, 163 avenue de Luminy, 13288 Marseille, France)
Publication:
Monthly Notices of the Royal Astronomical Society: Letters, Volume 426, Issue 1, pp. L76-L80. (MNRAS Homepage)
Publication Date:
10/2012
Origin:
WILEY
Astronomy Keywords:
radiative transfer, stars: evolution, stars: magnetars, supernovae: general, supernovae: individual: SN2007bi, PTF 09atu
Abstract Copyright:
© 2012 The Authors Monthly Notices of the Royal Astronomical Society © 2012 RAS
DOI:
10.1111/j.1745-3933.2012.01329.x
Bibliographic Code:
2012MNRAS.426L..76D

Abstract

Much uncertainty surrounds the origin of superluminous supernovae (SNe). Motivated by the discovery of the Type Ic SN 2007bi, we study its proposed association with a pair-instability SN (PISN). We compute stellar evolution models for primordial ˜200 M&sun; stars, simulating the implosion/explosion due to the pair-production instability, and use them as inputs for detailed non-local thermodynamic equilibrium time-dependent radiative transfer simulations that include non-local energy deposition and non-thermal processes. We retrieve the basic morphology of PISN light curves from red supergiant, blue supergiant and Wolf-Rayet (WR) star progenitors. Although we confirm that a progenitor 100 M&sun; helium core (PISN model He100) fits well the SN 2007bi light curve, the low ratios of its kinetic energy and 56Ni mass to the ejecta mass, similar to standard core-collapse SNe, conspire to produce cool photospheres, red spectra subject to strong line blanketing and narrow-line profiles, all conflicting with SN 2007bi observations. He-core models of increasing 56Ni-to-ejecta mass ratio have bluer spectra, but still too red to match SN 2007bi, even for model He125 - the effect of 56Ni heating is offset by the associated increase in blanketing. In contrast, the delayed injection of energy by a magnetar represents a more attractive alternative to reproduce the blue, weakly blanketed and broad-lined spectra of superluminous SNe. The extra heat source is free of blanketing and is not explicitly tied to the ejecta. Experimenting with an ˜9 M&sun; WR-star progenitor, initially exploded to yield an ˜1.6 B SN Ib/c ejecta but later influenced by tunable magnetar-like radiation, we produce a diversity of blue spectral morphologies reminiscent of SN 2007bi, the peculiar Type Ib SN 2005bf and superluminous SN 2005ap-like events.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints