High-resolution X-ray spectroscopy of the supernova remnant N132D

Details High-resolution X-ray spectroscopy of the supernova remnant N132D High-resolution X-ray spectroscopy of the supernova remnant N132D

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...414..219h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 414, no. 1, p. 219-229.

Astronomy and Astrophysics

Astrophysics

29

Focal Plane Devices, Interstellar Matter, Magellanic Clouds, Nonequilibrium Ionization, Supernova Remnants, X Ray Spectroscopy, Heao 2, High Resolution, Spectral Resolution

Scientific paper

A joint nonequilibrium ionization analysis of spectral data from the Einstein Observatory of the SNR N132D in the LMC is presented on the basis of data from the Focal Plane Crystal Spectrometer (FPCS) and the Solid State Spectrometer (SSS), and lower spectral resolution data from the IPC and the 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. Measured line widths for the oxygen lines suggest Doppler broadening that is roughly consistent with optically measured expansion velocities of 2250 km/s. At the SSS/IPC temperature, FPCS flux ratios constrain the O/Fe abundance to be at least 1.9 times its solar value and the O/Ne abundance to be 0.2-1.0 times its solar value. Models for remnants with progenitor masses of 20 and 25 solar masses are completely consistent with the data, while remnants with progenitor masses of 13 and 15 solar masses can be made consistent if the progenitors are required to eject a large fraction of their iron cores.

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