High-Resolution X-Ray Spectroscopy of the Accretion Disk Corona Source 4U 1822-37

Details High-Resolution X-Ray Spectroscopy of the Accretion Disk Corona Source 4U 1822-37 High-Resolution X-Ray Spectroscopy of the Accretion Disk Corona Source 4U 1822-37

2001-07-13

arxiv.org/abs/astro-ph/0107247v1

Astrophys.J. 557 (2001) L101

Astronomy and Astrophysics

Astrophysics

12 pages, 6 figures; Accepted for publication in ApJ Letters

Scientific paper

10.1086/323343

We present a preliminary analysis of the X-ray spectrum of the accretion disk corona source, 4U 1822-37, obtained with the High Energy Transmission Grating Spectrometer onboard the Chandra X-ray Observatory. We detect discrete emission lines from photoionized iron, silicon, magnesium, neon, and oxygen, as well as a bright iron fluorescence line. Phase-resolved spectroscopy suggests that the recombination emission comes from an X-ray illuminated bulge located at the predicted point of impact between the disk and the accretion stream. The fluorescence emission originates in an extended region on the disk that is illuminated by light scattered from the corona.

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