X-ray Absorption And Emission In Accretion Disks Of Bright Lmxbs

Details X-ray Absorption And Emission In Accretion Disks Of Bright Lmxbs X-ray Absorption And Emission In Accretion Disks Of Bright Lmxbs

Mar 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008head...10.1016s&link_type=abstract

American Astronomical Society, HEAD meeting #10, #10.16

Astronomy and Astrophysics

Astrophysics

Scientific paper

Compact binaries containing neutron stars and black holes emit luminous X-ray continua emanating from the central region of accretion. We traditionally model these X-ray spectra with radiative continuum processes added by some radiative reprocessing, in most cases Compton scattering and some additional isolated line features. High resolution X-ray spectrometers now enable us to recognize reprocessing in a much more sensitive fashion and we can use these X-ray continua to diagnose the conditions in the accretion disk through illumination and absorption. In many systems containing black holes powerful winds have been recognized through resonance line absorption and in a few X-ray binaries signatures of radiative heating of accretion disk atmospheres and coronae have been studied in some detail, some exhibiting warm absorbers as well. The bulk of sources, however, remained fairly devoid of such signatures, specifically the bright Z sources. This perception seems to be changing. A recent long exposed HETG observation of the prototype Z source Cyg X-2 not only shows lines from highly ionized ions, but also indicates a large dynamic range in line widths. We present analysis results from these spectra and compare them to previously obtained results from accretion disk coronal sources such as 4U 1822-37, Her X-1, EXO 0748-76, and Cir X-1 as well as the disk lines in the compact binary pulsar 4U 1626-67.
This work was supported by NASA through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 for the Chandra X-Ray Center and Science Instruments.

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