Other
Scientific paper
May 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.3904h&link_type=abstract
American Astronomical Society, 180th AAS Meeting, #39.04; Bulletin of the American Astronomical Society, Vol. 24, p.790
Other
1
Scientific paper
We present high spectral resolution X-ray data for supernova remnant N132D in the Large Magellanic Cloud obtained with the Focal Plane Crystal Spectrometer (FPCS) and the Solid State Spectrometer (SSS) on the Einstein Observatory. We also use lower spectral resolution data obtained with the Einstein's Imaging Proportional Counter (IPC) and Monitor Proportional Counter (MPC). The FPCS detected individual emission lines of O VII, O VIII, Ne IX, Ne X, Fe XVII, and possibly Fe XX, with the O VIII Ly alpha line alone contributing more than 10\ total unabsorbed X-ray luminosity. Ratios of measured line fluxes are used in conjunction with a simple model for emission from a plasma that is not in collisional ionization equilibrium to constrain the plasma temperature and ionization age. Spectral fits of this model to SSS and IPC data give a temperature of 7.4 times 10(6) K and an ionization age of 4.8 times 10(3) cm(-3) yr which are consistent with the FPCS results. These results are used to constrain the O/Fe abundance which is enhanced at least 5 times over its solar value and the Ne/O abundance which is 1--4 times its solar value. Comparison of these abundance ratios to those calculated for the ejecta of Type II supernovae mixed with an ambient medium with the abundance structure of the Large Magellanic Cloud suggests that the mass of the progenitor was about 20 Msun , a result consistent with indications from optical observations that N132D is the remnant of a Type II supernova explosion of a massive star. Finally, we point out that while oxygen emission dominates the X-ray emission, the SSS and IPC fits indicate that the abundances of oxygen and other heavy elements relative to the light elements are below both their solar value and their mean values for the LMC.
Canizares Calude R.
Hughes John Patrick
Hwang Una
Markert Thomas H.
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