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X-rays from Supernova Remnants
, 2002 A summary of X-ray observations of supernova remnants is presented including the explosion fragment A of the Vela SNR, Tycho, N132D, RX J0852-4622, the Crab Nebula and the 'bulls eye', and SN 1987A, high-lighting the progress made with Chandra and XMM ...
Aschenbach, B.
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New insights into the physical state of gaseous nebulae [PDF]
The impact of knowledge of H II regions, planetary nebulae and supernova remnants due to International Ultraviolet Explorer is examined. The more relevant aspects related to the physical conditions of gaseous nebulae are reviewed.
Peimbert, M.
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Dust in supernova remnants [PDF]
Proceedings of The Life Cycle of Dust in the Universe: Observations, Theory, and Laboratory Experiments — PoS(LCDU2013), 2014 openaire +3 more sources
Supernovae and Their Remnants [PDF]
, 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
Nino Panagia, William P. Blair
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Supernovae and supernova remnants [PDF]
, 2001 A 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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Supernovae and Their Remnants [PDF]
, 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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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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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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Observations of Supernova Remnants
Annual Review of Astronomy and Astrophysics, 1984Les restes de supernovae jeune: RSN riches en metaux CasA, restes de type I Tycho, le Crabe. Les restes d'âge intermediaire: la Boucle du Cygne. Les vieux restes de supernovae; l'eperon polaire nord. Les restes de supernovae de transition.
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