Using X-ray Emission from Core-Collapse Supernova Shocks to Probe Circumstellar Environments

Details Using X-ray Emission from Core-Collapse Supernova Shocks to Probe Circumstellar Environments Using X-ray Emission from Core-Collapse Supernova Shocks to Probe Circumstellar Environments

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..937..436k&link_type=abstract

SUPERNOVA 1987A: 20 YEARS AFTER: Supernovae and Gamma-Ray Bursters. AIP Conference Proceedings, Volume 937, pp. 436-439 (2007).

Physics

1

X-Ray, Supernovae, Circumstellar Shells, Clouds, And Expanding Envelopes, Circumstellar Masers

Scientific paper

In supernova (SN), the ejected material drives powerful shock fronts into the stellar winds of progenitor stars at speeds of tens of thousand kilometers per second. A layer of shocked circumstellar material (CSM) and ejected material develops that can be observed in X-ray emission due to the high associated temperatures (106-109 K). Analysis of the interaction between the ejected material and CSM leads to information on the temperature and density structure as well as the mass loss rate of the progenitor star. As the SN blast wave moves to ever increasing radii, it offers an opportunity to study older and older stellar winds over periods of tens of thousands of years in the history of the progenitors. To date there have been 32 SN detected in X-rays in the past ~30 years, and a detailed study offers interesting new insights into the stellar wind history of the progenitor stars. The analysis shows that all young (<40 years) X-ray emitting SN detected have strikingly similar CSM density profiles, ranging more than 9 orders of magnitude (0.1-108 cm-3) over a distance range of 7 orders of magnitude from the sites of the explosions.

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