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Title:
The Thermal Composite Supernova Remnant Kesteven 27 as Viewed by Chandra: Shock Reflection from a Cavity Wall
Authors:
Chen, Yang; Seward, Frederick D.; Sun, Ming; Li, Jiang-tao
Affiliation:
AA(Department of Astronomy, Nanjing University, Nanjing, 210093 Jiangsu, China.), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138.), AC(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824.), AD(Department of Astronomy, Nanjing University, Nanjing, 210093 Jiangsu, China.)
Publication:
The Astrophysical Journal, Volume 676, Issue 2, pp. 1040-1049. (ApJ Homepage)
Publication Date:
04/2008
Origin:
UCP
ApJ Keywords:
ISM: individual (Kesteven 27 ), ISM: individual ( G327.4+0.4), Radiation Mechanisms: Thermal, Shock Waves, ISM: Supernova Remnants, X-Rays: ISM
DOI:
10.1086/525240
Bibliographic Code:
2008ApJ...676.1040C

Abstract

We present a spatially resolved spectroscopic study of the thermal composite supernova remnant Kes 27 with Chandra. The X-ray spectrum of Kes 27 is characterized by K lines from Mg, Si, S, Ar, and Ca. The X-ray-emitting gas is found to be enriched in sulfur and calcium. The broadband and tricolor images show two incomplete shell-like features in the northeastern half and brightness fading with increasing radius to the southwest. There are over 30 unresolved sources within the remnant. None shows characteristics typical of a young neutron star. The maximum diffuse X-ray intensity coincides with a radio-bright region along the eastern border. In general, gas in the inner region is at higher temperature, and the emission is brighter, than that in the outer region. The gas in the remnant appears to be near ionization equilibrium. The overall morphology can be explained by the evolution of the remnant in an ambient medium with a density enhancement from west to east. We suggest that the remnant was born in a preexisting cavity and that the bright inner emission is due to the reflection of the initial shock from the dense cavity wall. This scenario may provide a new candidate mechanism to explain the X-ray morphology of other thermal composite supernova remnants.
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