Super-Luminous Type Ic Supernovae: Catching a magnetar by the tail

Please use this identifier to cite or link to this item: https://ir.lib.ncu.edu.tw/handle/987654321/101010

Title:	Super-Luminous Type Ic Supernovae: Catching a magnetar by the tail
Authors:	陳婷琬;Inserra, C;Smartt, S J;JERKSTRAND, A;Valenti, S;Fraser, M;Wright, D;Smith, K;Chen, T-W;Kotak, R;Pastorello, A
Contributors:	理學院天文研究所
Keywords:	ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;COBALT 56;Deposition;DETECTION;DIAGRAMS;Diffusion;Ejecta;ENERGY ABSORPTION;ENERGY LOSSES;Explosions;GALAXIES;HELIUM;INFRARED SPECTRA;LUMINOSITY;MASS;Mathematical models;NICKEL 56;NUCLEAR DECAY;PEAKS;Photometry;PTF11rks;RED SHIFT;SN 2011ke;SN 2011kf;SN 2012il;SPIN;stars: magnetars;SUPERNOVAE;supernovae: general;supernovae: individual (PTF10hgi
Date:	2013-06-20
Issue Date:	2026-04-21 14:20:56 (UTC+8)
Publisher:	IOP Publishing Ltd.;United States
Abstract:	摘要： We report extensive observational data for five of the lowest redshift Super-Luminous Type Ic Supernovae (SL-SNe Ic) discovered to date, namely, PTF10hgi, SN2011ke, PTF11rks, SN2011kf, and SN2012il. Photometric imaging of the transients at +50 to +230 days after peak combined with host galaxy subtraction reveals a luminous tail phase for four of these SL-SNe. A high-resolution, optical, and near-infrared spectrum from xshooter provides detection of a broad Hei X10830 emission line in the spectrum (+50 days) of SN2012il, revealing that at least some SL-SNe Ic are not completely helium-free. At first sight, the tail luminosity decline rates that we measure are consistent with the radioactive decay of super(56)Co, and would require 1-4 M sub([middot in circle]) of super(56)Ni to produce the luminosity. These super(56)Ni masses cannot be made consistent with the short diffusion times at peak, and indeed are insufficient to power the peak luminosity. We instead favor energy deposition by newborn magnetars as the power source for these objects. A semi-analytical diffusion model with energy input from the spin-down of a magnetar reproduces the extensive light curve data well. The model predictions of ejecta velocities and temperatures which are required are in reasonable agreement with those determined from our observations. We derive magnetar energies of 0.4 [<, ~] E(10 super(51) erg) [<, ~] 6.9 and ejecta masses of 2.3 [<, ~] M sub(ej)(M sub([middot in circle])) [<, ~] 8.6. The sample of five SL-SNe Ic presented here, combined with SN 2010gx-the best sampled SL-SNe Ic so far-points toward an explosion driven by a magnetar as a viable explanation for all SL-SNe Ic. 出版者： United States 出版日期： 2013-06-20 出處： The Astrophysical journal, 2013-06, Vol.770 (2), p.1-28 資源來源： Institute of Physics Journals 識別號： ISSN: 0004-637X 識別號： ISSN: 1538-4357 識別號： EISSN: 1538-4357 識別號： DOI: 10.1088/0004-637X/770/2/128
Appears in Collections:	[Graduate Institute of Astronomy] journal & Dissertation

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