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Superluminous supernovae: ^(56)Ni power versus magnetar radiation

Dessart, Luc and Hillier, D. John and Waldman, Roni and Livne, Eli and Blondin, Stéphane (2012) Superluminous supernovae: ^(56)Ni power versus magnetar radiation. Monthly Notices of the Royal Astronomical Society: Letters, 426 (1). L76-L80. ISSN 1745-3933.

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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_⊙ 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_⊙ helium core (PISN model He100) fits well the SN 2007bi light curve, the low ratios of its kinetic energy and ^(56)Ni 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 ^(56)Ni-to-ejecta mass ratio have bluer spectra, but still too red to match SN 2007bi, even for model He125 – the effect of ^(56)Ni 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_⊙ 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.

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Additional Information:© 2012 The Authors. Monthly Notices of the Royal Astronomical Society © 2012 RAS. Accepted 2012 August 5. Received 2012 July 2; in original form 2012 May 20. Article first published online: 10 Sep. 2012. LD and SB acknowledge support from European-Community grant PIRG04-GA-2008-239184 and from ANR grant 2011-Blanc-SIMI- 5-6-007-01. DJH acknowledges support from STScI theory grants HST-AR-11756.01.A and HST-AR-12640.01, and NASA theory grant NNX10AC80G.
Funding AgencyGrant Number
European CommunityPIRG04-GA-2008-239184
ANR grant2011-Blanc-SIMI-5-6-007-01
STScI Theory GrantHST-AR-11756.01.A
STScI Theory GrantHST-AR-12640.01
NASA Theory GrantNNX10AC80G
Subject Keywords: radiative transfer; stars: evolution; stars: magnetars; supernovae: general; supernovae: individual: SN2007bi, PTF 09atu
Issue or Number:1
Record Number:CaltechAUTHORS:20121114-114118401
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Official Citation:Dessart, L., Hillier, D. J., Waldman, R., Livne, E. and Blondin, S. (2012), Superluminous supernovae: 56Ni power versus magnetar radiation. Monthly Notices of the Royal Astronomical Society: Letters, 426: L76–L80. doi: 10.1111/j.1745-3933.2012.01329.x
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:35460
Deposited By: Ruth Sustaita
Deposited On:14 Nov 2012 21:19
Last Modified:03 Oct 2019 04:28

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