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H and He in stripped-envelope SNe – how much can be hidden?

Published online by Cambridge University Press:  05 September 2012

S. Hachinger ,
P. A. Mazzali ,
S. Taubenberger ,
W. Hillebrandt ,
K. Nomoto  and
D. N. Sauer
S. Hachinger
Affiliation:
Istituto Nazionale di Astrofisica – OA Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy email: stephan.hachinger@oapd.inaf.it Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
P. A. Mazzali
Affiliation:
Istituto Nazionale di Astrofisica – OA Padova, vicolo dell'Osservatorio 5, 35122 Padova, Italy email: stephan.hachinger@oapd.inaf.it Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
S. Taubenberger
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
W. Hillebrandt
Affiliation:
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, 85748 Garching, Germany
K. Nomoto
Affiliation:
Kavli Institute for the Physics and Mathematics of the Universe, University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8583, Japan Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
D. N. Sauer
Affiliation:
Department of Astronomy, Stockholm University, Alba Nova University Centre, SE-10691 Stockholm, Sweden Meteorologisches Institut, Universität München, Theresienstr. 37, 80333 München, Germany
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Abstract

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H and He features in photospheric spectra have rarely been used to constrain the structure of Type IIb/Ib/Ic supernovae (SNe IIb/Ib/Ic). The lines have to be modelled with a detailed non-local-thermodynamic-equilibrium (NLTE) treatment, including effects uncommon in stars. Once this is done, however, one obtains valuable hints on the characteristics of progenitors and explosions (composition, explosion energy, . . .). We have extended a radiative transfer code to compute synthetic spectra of SNe IIb, Ib and Ic. Here, we discuss our first larger set of models, focusing on the question: How much H/He can be hidden (i.e. remain undetected in photospheric spectra) in SNe Ib/Ic? For the SNe studied (relatively low Mej = 1. . .3 M⊙), we find a limit of MHe ≲ 0.1 M⊙ in SNe Ic (no unambiguous He lines). Stellar evolution models for single stars normally always yield higher masses. We suggest that low- or moderate-mass SNe Ic result from efficient envelope stripping in binaries. We propose similar studies on H/He in high-mass and extremely aspherical SNe, and observations covering the region of He I λ 20581.

Keywords

supernovae: generalsupernovae: individual (SN 2008ax, SN 1994I)techniques: spectroscopicradiative transfer
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 122 - 125
Copyright
Copyright © International Astronomical Union 2012

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