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          Institute: MPI für Radioastronomie     Collection: Publikationen des MPI für Radioastronomie     Display Documents

ID: 10866.0, MPI für Radioastronomie / Publikationen des MPI für Radioastronomie
SN 1993J VLBI. II. Related changes of the deceleration, flux density decay, and spectrum
Authors:Bartel, N.; Bietenholz, M. F.; Rupen, M. P.; Beasley, A. J.; Graham, D. A.; Altunin, V. I.; Venturi, T.; Umana, G.; Cannon, W. H.; Conway, J. E.
Date of Publication (YYYY-MM-DD):2002-12-10
Title of Journal:Astrophysical Journal
Journal Abbrev.:Astrophys. J.
Issue / Number:1
Start Page:404
End Page:426
Review Status:Peer-review
Audience:Experts Only
Abstract / Description:Phase-referenced multifrequency VLBI observations of supernova 1993J in the nearby galaxy M81 at 34 epochs from t = 30 to similar to3000 days after shock breakout show the detailed characteristics of the non self-similar expansion. For the first year, the supernova expanded almost freely, with the outer radius of the radio shell r(o) proportional to t(m(t)) and m(t) = 0.919 +/- 0.019. During the following 4 years the deceleration grew to m(t) = 0.781 +/- 0.009, the expansion velocity slowed down by about half from originally v(0) similar to17,200 km s(-1) to just similar to8900 km s(-1), and the supernova swept up a mass of similar to0.3 M-.. Momentum conservation suggests that this mass is about equal to the mass of the shocked ejecta, likely composed of all the low-mass envelope of the progenitor left over after mass transfer to a purported binary companion, therefore supporting the binary scenario. Subsequently the deceleration changed again, this time decreasing to m(t) = 0.860 +/- 0.011 from t = 5 to 8 yr, consistent with hydrodynamic simulations. This late upturn of m(t) may be caused by the massive inner ejecta, which have reached the increasingly decelerated shocked ejecta, passing now through the reverse shock and pushing the low-mass envelope. This upturn of m(t) is mirrored by changes in the slope of the radio light curves and a flattening of the radio spectra, all consistent with power laws, with spectral indices changing from alpha = -0.85 +/- 0.03 to -0.64 +/- 0.03. The magnetic field in the radio shell region is inferred to decrease from originally proportional to r(o)(-0.99) to proportional to r(o)(-1.45) toward the end of our observations. After 7 years the radio light curves start to drop rapidly, suggesting that the supernova is now expanding into a zone of the circumstellar medium with a steep density profile.
Free Keywords:supernovae : individual (SN 1993J); techniques : interferometric
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Radioastronomie
External Affiliations:York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada; York Univ, Dept Phys & Astron, N York, ON M3J 1P3, Canada; Natl Radio Astron Observ, Socorro, NM 87801 USA; Owens Valley Radio Observ, CARMA, Pig Pine, CA 93513 USA; Max Planck Inst Radioastron, D-53121 Bonn, Germany; CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA; CNR, Inst Radioastron, I-40129 Bologna, Italy; CNR, Inst Radioastron, I-96017 Noto, Italy; CRESTech, Space Geodynam Lab, Toronto, ON M3J 3K1, Canada; Chalmers Univ Technol, Onsala Space Observ, S-43992 Onsala, Sweden
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