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Radiation Hydrodynamical Models for Type I Superluminous Supernovae: Constraints on Progenitors and Explosion Mechanisms

Published online by Cambridge University Press:  28 July 2017

Ken’ichi Nomoto ,
Alexey Tolstov ,
Elena Sorokina ,
Sergei Blinnikov ,
Melina Bersten  and
Tomoharu Suzuki
Ken’ichi Nomoto
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan Hamamatsu Professor email: [email protected]
Alexey Tolstov
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan
Elena Sorokina
Affiliation:
Sternberg Astronomical Institute, M.V.Lomonosov Moscow State U., 119991 Moscow, Russia
Sergei Blinnikov
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan Institute for Theoretical and Experimental Physics, 117218 Moscow, Russia
Melina Bersten
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo, Kashiwa, Chiba 277-8583, Japan Instituto de Astrofisica La Plata, 1900 La Plata, Argentina
Tomoharu Suzuki
Affiliation:
College of Engineering, Chubu University, Kasugai, Aichi 487-8501, Japan
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Abstract

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The physical origin of Type-I (hydrogen-less) superluminous supernovae (SLSNe-I), whose luminosities are 10 to 500 times higher than normal core-collapse supernovae, remains still unknown. Thanks to their brightness, SLSNe-I would be useful probes of distant Universe. For the power source of the light curves of SLSNe-I, radioactive-decays, magnetars, and circumstellar interactions have been proposed, although no definitive conclusions have been reached yet. Since most of light curve studies have been based on simplified semi-analytic models, we have constructed multi-color light curve models by means of detailed radiation hydrodynamical calculations for various mass of stars including very massive ones and large amount of mass loss. We compare the rising time, peak luminosity, width, and decline rate of the model light curves with observations of SLSNe-I and obtain constraints on their progenitors and explosion mechanisms. We particularly pay attention to the recently reported double peaks of the light curves. We discuss how to discriminate three models, relevant models parameters, their evolutionary origins, and implications for the early evolution of the Universe.

Keywords

magnetarstellar mass losssupernovaesuperluminous supernovae
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 39 - 43
Copyright
Copyright © International Astronomical Union 2017 

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