Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011head...12.3422d&link_type=abstract
American Astronomical Society, HEAD meeting #12, #34.22
Astronomy and Astrophysics
Astrophysics
Scientific paper
The interaction of SN 1987A with its environment gives rise to X-ray emission from multiple components of the system: the H_II region, the dense protrusions of the equatorial ring (ER) including clumpy ER material, and, at late times, the reverse-shocked SN ejecta itself.
Deep Chandra and XMM gratings observations span the period from late 1999 to the present. The HETG observation in 1999 showed very broad lines with FWHM of order 7000 km/s (Michael et al. 2002); at this time the blast wave was primarily interacting with the H_II region around the progenitor. Since then, the X-ray emission has been increasingly dominated by narrower components as the blast wave encounters the dense ER. Even so, the grating data suggest that flux from the H_II region is still present, indicated by a very-broad component in the grating spectra. We find that deep HETG 2007 and 2011 data are better fit when of order 0.2 of the flux comes from a component with FWHM around 9000 km/s.
Based on this, the observed light curves in the 0.5-2 and 3-10 keV bands are modeled as the weighted sum of the non-equilibrium-ionization (NEI) X-ray emission from two simple 1D hydrodynamic simulations: one for the very-broad H_II interaction and one for the dense ER collision. Using these simple models we can better understand and interpret the X-ray emission components and their properties (e.g., abundances), predict future light curve changes under different model assumptions, and set initial parameters for a multi-D model of SN 1987A's interaction.
Support for this work was provided by NASA contract NAS8-03060 to the Smithsonian Astrophysical Observatory (SAO) and SAO sub-contracts TM9-0004X to VVD (U Chicago) and SV3-73016 to MIT for support of the CXC.
Canizares Calude R.
Dewey Daniel
Dwarkadas Vikram V.
Haberl Franck
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