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A binary merger product as the direct progenitor of a Type II-P supernova
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Abundances in supernova remnants
AIP Conference Proceedings, 1984This paper outlines the abundances one may expect to observe as the result of an explosion of the evolved star that is the progenitor of a supernova. (AIP)
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Space Science Reviews, 1985
A progress report is given on our current interpretation of the X-ray emission from supernova remnants. Previous results from earlier experiments, the Einstein Observatory in particular, are reviewed and supplemented by the most recent data from the Exosat mission for a selection of remnants (Puppis-A, Cas-A, SN 1006, RCW103, W49B).
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A progress report is given on our current interpretation of the X-ray emission from supernova remnants. Previous results from earlier experiments, the Einstein Observatory in particular, are reviewed and supplemented by the most recent data from the Exosat mission for a selection of remnants (Puppis-A, Cas-A, SN 1006, RCW103, W49B).
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Supernovae and supernova remnants
2001A supernova explosion is among the most dramatic events that can be seen. The term ‘supernova’ is somewhat misleading, as such an event represents not a new star (that is, a ‘nova’), but instead the end of a star’s life. Nuclear fusion, the energy source of the stars, creates heavier elements from lighter elements.
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Evolution of Supernova Remnants. I. Interacting Supernova Remnants
Publications of the Astronomical Society of Japan, 1978Abstract The evolution and structure of two interacting supernova remnants (SNRs) are calculated by use of a time-dependent two-dimensional hydrodynamic code. The interactions of two SNRs are simulated in such a way that at a time t0 after the first supernova explosion, the second supernova explosion occurs at the distance D and two SNRs
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2004
Abstract An explosion eventually occurs in a highly evolved single star of sufficient mass or in a white dwarf that has accreted enough material from its companion in a binary system. Explosions give some individual stars optical luminosities that for a couple of months are more than a billion times that of the Sun.
T W Hartquist, J E Dyson, D P Ruffle
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Abstract An explosion eventually occurs in a highly evolved single star of sufficient mass or in a white dwarf that has accreted enough material from its companion in a binary system. Explosions give some individual stars optical luminosities that for a couple of months are more than a billion times that of the Sun.
T W Hartquist, J E Dyson, D P Ruffle
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Supernovae and Supernova Remnants
1983Supernovae are the result of explosions which terminate the life of massive stars. The amount of energy released by the supernovae in our galaxy is so large that these explosions provide the dominant energy for the heating of the hot (T ≳ 106 K) IS component and for the kinetic energy of the large scale motions of the interstellar clouds.
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1987
Supernovae (SNe) and supernova remnants (SNRs) represent an important area of research in astrophysics because they are central to our understanding of such diverse fields as the late stages of stellar evolution, mass loss from late-type stars, nucleosynthesis, and interstellar medium processes and abundances. In addition, they provide a laboratory for
William P. Blair, Nino Panagia
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Supernovae (SNe) and supernova remnants (SNRs) represent an important area of research in astrophysics because they are central to our understanding of such diverse fields as the late stages of stellar evolution, mass loss from late-type stars, nucleosynthesis, and interstellar medium processes and abundances. In addition, they provide a laboratory for
William P. Blair, Nino Panagia
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Supernovae and Supernova Remnants
Annual Review of Astronomy and Astrophysics, 1988Kurt W. Weiler, Richard A. Sramek
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1988
Supernovas can be divided into two distinct classes on the basis of their spectra. Supernovae of type I (SNI) exhibit no hydrogen lines whereas those of type II (SNII) do show hydrogen lines in their spectra. Historically (Baade 1958) SNI have, with the usual perversity of astronomical nomenclature, been assigned to Population II and SNII to Population
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Supernovas can be divided into two distinct classes on the basis of their spectra. Supernovae of type I (SNI) exhibit no hydrogen lines whereas those of type II (SNII) do show hydrogen lines in their spectra. Historically (Baade 1958) SNI have, with the usual perversity of astronomical nomenclature, been assigned to Population II and SNII to Population
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