Modeling the stellar contribution to the Galactic component of the diffuse soft X-ray background. I - Background fluxes and number counts

Details Modeling the stellar contribution to the Galactic component of the diffuse soft X-ray background. I - Background fluxes and number counts Modeling the stellar contribution to the Galactic component of the diffuse soft X-ray background. I - Background fluxes and number counts

Jun 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...391..667k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 391, no. 2, June 1, 1992, p. 667-684. Research supported by MURST and ASI.

Other

22

Cosmic X Rays, Emission Spectra, Main Sequence Stars, Stellar Luminosity, Stellar Radiation, Diffuse Radiation, Einstein Equations, X Ray Spectra

Scientific paper

A combination of a stellar Galaxy model based on optical data, stellar X-ray luminosity functions derived from the full Einstein base, and a model for X-ray absorption derived from hydrogen column densities are used to estimate the contribution to the diffuse soft X-ray background flux from the main-sequence A, F, G, K, and M stars, and RS CVn stars, at various energies ranging from 0.1 to about 5 keV. Previous discrepancies between earlier estimates of the stellar contribution to the diffuse soft X-ray background are resolved; this stellar contribution to the diffuse soft X-ray background is found to be under 3 percent for photon energies less than energy I and J bands (about 0.8-2 keV), at a threshold sensitivity for point source detection about 10 exp -10 ergs/s sq cm. At low latitudes, stellar contribution estimates are less than 3 percent below 0.3 keV, 7-40 percent in the medium-energy bands, and 27-70 percent in the I and J bands. It is shown that while dM stars are the major contributors to the diffuse stellar flux, other stellar types contribute as much as 40 percent of this flux at the higher energies in the passband studied.

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