A model of the pre-Sedov expansion phase of supernova remnant-ambient plasma coupling and X-ray emission from SN 1987A

Journal Article · Fri Jun 01 04:00:00 EDT 1990 · Astrophysical Journal; (USA)

DOI:https://doi.org/10.1086/168862· OSTI ID:6934247

Spicer, D S; Maran, S P; Clark, R W ^[1]

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1. NASA, Goddard Space Flight Center, Greenbelt, MD (USA) Naval Research Laboratory, Washington, DC (USA)

This paper examines the mechanism responsible for coupling supernova (SN) remnant to the ambient medium during the pre-Sedov or the so-called free expansion phase, immediately following the progenitor explosion. A theory is developed for the interaction of an SN piston with the ambient medium during the pre-Sedov phase. The possibility of X-ray production by the high-speed portion of the piston during this phase is investigated. The relevant observations of high-energy emissions from the SN 1987A, including the X-ray spectrum, luminosity, and temporal development, are considered. It is shown that the commonly assumed snowplow model for SNR evolution is valid, because of the action of a variety of collisionless two-stream instabilities that permit the coupling of the ambient plasma with SNR. 68 refs.

• OSTI ID: 6934247
• Journal Information: Astrophysical Journal; (USA), Journal Name: Astrophysical Journal; (USA) Vol. 356; ISSN ASJOA; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC RADIO SOURCES
ELECTROMAGNETIC RADIATION
EMISSION SPECTRA
ERUPTIVE VARIABLE STARS
EXPANSION
EXPLOSIONS
FLUID MECHANICS
GALAXIES
HYDRODYNAMICS
INSTABILITY
IONIZING RADIATIONS
LUMINOSITY
MAGELLANIC CLOUDS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
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OPTICAL PROPERTIES
PHYSICAL PROPERTIES
PLASMA
PLASMA INSTABILITY
PLASMA MICROINSTABILITIES
RADIATIONS
SPECTRA
STABILITY
STAR EVOLUTION
STARS
SUPERNOVA REMNANTS
SUPERNOVAE
TWO-STREAM INSTABILITY
VARIABLE STARS
X RADIATION
X-RAY SPECTRA