Hostname: page-component-cd9895bd7-jn8rn Total loading time: 0 Render date: 2024-12-23T12:00:50.238Z Has data issue: false hasContentIssue false
  • English
  • Français

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: [email protected] 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: [email protected] 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
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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

References

Arcavi, I., et al. 2011, ApJ (Letters), 742, L18CrossRefGoogle Scholar
Cappellaro, E., Mazzali, P. A., Benetti, S., Danziger, I. J., Turatto, M., della Valle, M., & Patat, F. 1997, A&A, 328, 203Google Scholar
Chornock, R., et al. 2011, ApJ, 739, 41CrossRefGoogle Scholar
Corsi, A., et al. 2012, ApJ (Letters), 747, L5CrossRefGoogle Scholar
Eldridge, J. J., Langer, N., & Tout, C. A. 2011, MNRAS, 414, 3501CrossRefGoogle Scholar
Filippenko, A. V., et al. 1995, ApJ (Letters), 450, L11+CrossRefGoogle Scholar
Georgy, C., Meynet, G., Walder, R., Folini, D., & Maeder, A. 2009, A&A, 502, 611Google Scholar
Hachinger, S., Mazzali, P. A., Taubenberger, S., Hillebrandt, W., Nomoto, K., & Sauer, D. N. 2012, MNRAS, in press, doi: 10.1111/j.1365-2966.2012.20464.xCrossRefGoogle Scholar
Iwamoto, K., Nomoto, K., Hoflich, P., Yamaoka, H., Kumagai, S., & Shigeyama, T. 1994, ApJ (Letters), 437, L115CrossRefGoogle Scholar
Kasen, D., Nugent, P., Thomas, R. C., & Wang, L. 2004, ApJ, 610, 876CrossRefGoogle Scholar
Lucy, L. B. 1991, ApJ, 383, 308CrossRefGoogle Scholar
Lucy, L. B. 1999, A&A, 345, 211Google Scholar
Mazzali, P. A. 2000, A&A, 363, 705Google Scholar
Mazzali, P. A., et al. 2008, Science, 321, 1185CrossRefGoogle Scholar
Nomoto, K., Yamaoka, H., Pols, O. R., van den Heuvel, E. P. J., Iwamoto, K., Kumagai, S., & Shigeyama, T. 1994, Nature, 371, 227CrossRefGoogle Scholar
Sauer, D. N., Mazzali, P. A., Deng, J., Valenti, S., Nomoto, K., & Filippenko, A. V. 2006, MNRAS, 369, 1939CrossRefGoogle Scholar
Shigeyama, T., Suzuki, T., Kumagai, S., Nomoto, K., Saio, H., & Yamaoka, H. 1994, ApJ, 420, 341CrossRefGoogle Scholar
Stehle, M., Mazzali, P. A., Benetti, S., & Hillebrandt, W. 2005, MNRAS, 360, 1231CrossRefGoogle Scholar
Taubenberger, S., et al. 2011, MNRAS, 413, 2140CrossRefGoogle Scholar
Utrobin, V. P. 1996, A&A, 306, 219Google Scholar
Yoon, S., Woosley, S. E., & Langer, N. 2010, ApJ, 725, 940CrossRefGoogle Scholar