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Supernova 1993J in M81

Published online by Cambridge University Press:  13 May 2016

M. F. Bietenholz
Affiliation:
York University, Toronto, Ont., M3J 1P3, Canada
N. Bartel
Affiliation:
York University, Toronto, Ont., M3J 1P3, Canada
M. P. Rupen
Affiliation:
National Radio Astronomy Observatory, Socorro, NM 87801, USA
A. J. Beasley
Affiliation:
National Radio Astronomy Observatory, Socorro, NM 87801, USA
D. A. Graham
Affiliation:
Max-Planck-Institut für Radioastronomie, D-53121, Bonn, Germany
V. I. Altunin
Affiliation:
Jet Propulsion Laboratory, Pasadena, CA 91109, USA
T. Venturi
Affiliation:
Instituto di Radioastronomia, CNR, Bologna/Noto, Italy
G. Umana
Affiliation:
Instituto di Radioastronomia, CNR, Bologna/Noto, Italy
W. H. Cannon
Affiliation:
York University, Toronto, Ont., M3J 1P3, Canada CRESTech, Toronto, Ont., M3J 3K1, Canada
J. E. Conway
Affiliation:
Onsala Space Observatory, S-43992, Onsala, Sweden

Abstract

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Twenty-two consecutive VLBI images of supernova 1993J in the galaxy M81 taken over 7 years show, in unprecedented detail, the dynamic evolution of the expanding radio shell of an exploded star. High precision astrometry using phase-referencing shows that the supernova expands isotropically, and that its geometric center has a formal proper motion of 190±110 km s−1 w.r.t. the core of M81. Systematic changes in the images most likely reflect a pattern of inhomogeneities in the medium left over from the progenitor star, or possibly instabilities in the expanding shell. As the shockfront sweeps up the medium, it is progressively decelerated, and after 7 years it has slowed to less than 1/2 its original expansion velocity. SN1993J is likely now entering the early stages of the adiabatic phase common in much older supernova remnants.

Type
Supernovae, Pulsars, and the Interstellar Medium
Copyright
Copyright © Astronomical Society of the Pacific 2001 

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