X-ray studies of the supernova remnant N132D. I - Morphology

Details X-ray studies of the supernova remnant N132D. I - Morphology X-ray studies of the supernova remnant N132D. I - Morphology

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...314..103h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 314, March 1, 1987, p. 103-110.

Astronomy and Astrophysics

Astronomy

36

Magellanic Clouds, Supernova Remnants, X Ray Sources, Galactic Structure, H Ii Regions, Interstellar Radiation, Nebulae, X Ray Astronomy

Scientific paper

From studies of the X-ray image of the supernova remnant N132 D in the Large Magellanic Cloud, the author determines that the supernova explosion occurred within a cavity in the interstellar medium. As a possible explanation for the formation of such a cavity he considers the H II region of the precursor star, which gives an adequate fit if the precursor stellar type is later than B0. The author also derives limits on the age and explosion energy, assuming the applicability of the Sedov solution. Consistency with the dynamical age estimates from the high-velocity oxygen-rich optical filaments can be obtained with a cavity density of ≡0.01 cm-3 or less and an explosion energy of ≡1051ergs.

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