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Strongly decelerated expansion of SN 1979C

Marcaide, J. M. and Pérez-Torres, M. A. and Ros, E. and Alberdi, A. and Diamond, P. J. and Guirado, J. C. and Lara, L. and Van Dyk, S. D. and Weiler, K. W. (2002) Strongly decelerated expansion of SN 1979C. Astronomy & Astrophysics, 384 (2). pp. 408-413. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20180307-090126185

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Abstract

We observed SN 1979C in M100 on 4 June 1999, about twenty years after explosion, with a very sensitive four-antenna VLBI array at the wavelength of λ18 cm. The distance to M100 and the expansion velocities are such that the supernova cannot be fully resolved by our Earth-wide array. Model-dependent sizes for the source have been determined and compared with previous results. We conclude that the supernova shock was initially in free expansion for 6 ± 2 yrs and then experienced a very strong deceleration. The onset of deceleration took place a few years before the abrupt trend change in the integrated radio flux density curves. We estimate the shocked swept-up mass to be M_(sw) ~ 1.6 M_⊙, assuming a standard density profile for the CSM. Such a swept-up mass for SN 1979C suggests a mass of the hydrogen-rich envelope ejected at explosion no larger than M_(env) ~ 0.9 M_⊙. If SN 1979C originated in a binary star, the low value of M_(env) suggests that the companion of the progenitor star stripped off most of the hydrogen-rich envelope mass of the presupernova star prior to the explosion.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1051/0004-6361:20011794DOIArticle
https://www.aanda.org/articles/aa/abs/2002/11/aah3030/aah3030.htmlPublisherArticle
https://arxiv.org/abs/astro-ph/0201206arXivDiscussion Paper
ORCID:
AuthorORCID
Van Dyk, S. D.0000-0001-9038-9950
Additional Information:© 2002 ESO. Received: 20 July 2001. Accepted: 11 December 2001. We are grateful to A. Kraus for the help provided during the observations and the flux density measurements on PKS B1157+156. This work has been partially supported by the Spanish DGICYT Grants No. PB96-0782 and PB97-1164. NRAO is operated under license by Associated Universities, Inc., under cooperative agreement with NSF. We acknowledge support from the European Commission's TMR-LSF programme, Contract No. ERBFMGEST950012. JMM is grateful to the Max-Planck Institut für Radioastronomie for the support received for this research during his visit. KWW wishes to thank the Office of Naval Research for the 6.1 funding supporting this work.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Departmento Governmental de Investigaciónes Cientificas y Técnológicas (DGICYT)PB96-0782
Departmento Governmental de Investigaciónes Cientificas y Técnológicas (DGICYT)PB97-1164
NSFUNSPECIFIED
European CommissionERBFMGEST950012
Office of Naval Research (ONR)UNSPECIFIED
Max Planck Institute for Astronomy (MPIA)UNSPECIFIED
Subject Keywords:techniques: interferometric - supernovae: individual: SN 1979C - ISM: supernova remnants - radio continuum: stars - galaxies: individual: M100
Issue or Number:2
Record Number:CaltechAUTHORS:20180307-090126185
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180307-090126185
Official Citation:J. M. Marcaide, M. A. Pérez-Torres, E. Ros, A. Alberdi, P. J. Diamond, J. C. Guirado, L. Lara, S. D. Van Dyk and K. W. Weiler A&A, 384 2 (2002) 408-413 DOI: https://doi.org/10.1051/0004-6361:20011794
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:85169
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:07 Mar 2018 17:20
Last Modified:03 Oct 2019 19:27

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