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Title:
The X-ray surface brightness of Kepler's supernova remnant
Authors:
White, R. L.; Long, K. S.
Affiliation:
AA(Columbia University, New York, NY), AB(Columbia University, New York, NY)
Publication:
Astrophysical Journal, Part 1, vol. 264, Jan. 1, 1983, p. 196-205. (ApJ Homepage)
Publication Date:
01/1983
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
INTERSTELLAR GAS, RADIANT FLUX DENSITY, SUPERNOVA REMNANTS, X RAY IMAGERY, X RAY SOURCES, ADIABATIC CONDITIONS, BRIGHTNESS DISTRIBUTION, GAS DENSITY, GAS EXPANSION, HEAO 2, INTERSTELLAR EXTINCTION, LUMINOSITY
DOI:
10.1086/160586
Bibliographic Code:
1983ApJ...264..196W

Abstract

The first X-ray images of Kepler's supernova remnant (SN Ophiuchi 1604) are presented, and consequences for SNR models are discussed. Observations made with the Einstein Observatory Imaging Proportional Counter and High Resolution Imager show the remnant to be circular, with a strong shell brighter in the north than in the south. A flux of 1.2 x 10 to the -10th ergs/sq cm per sec was measured in the 0.15-4.5 keV region, which corresponds to an X-ray luminosity of 1.0 x 10 to the 36th ergs/sec at a distance of 5 kpc and an interstellar medium density of 2.8 x 10 to the 21st/sq cm. The X-ray observations do not allow the determination of whether the SNR is in the adiabatic or free expansion phase, but in either case it is shown that the mean ISM density must be greater than about 0.1/cu cm. In addition, the density of the X-ray emitting gas must be high, and its electron temperature must be fairly low. The high ISM densities derived for Kepler's SNR and other SNRs thus suggest an atypical ISM, possibly influenced by mass lost from the pre-supernova star.

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