Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.4228j&link_type=abstract
American Astronomical Society, HEAD meeting #11, #42.28; Bulletin of the American Astronomical Society, Vol. 41, p.729
Astronomy and Astrophysics
Astronomy
Scientific paper
4U1822-371 is one of the proto-type accretion disk corona sources (ADCs) with an orbital period of about 5.6 hours. High resolution X-ray spectroscopic observations not only offer us copious spectroscopic information about orbital and disk dynamics, but also quantitative constraints on the physical properties of the plasma. 4U 1822-371 is specifically interesting because of its very high inclination angle of 83 degrees, allowing for an almost full edge-on view. We observed the X-ray source twice in May 2008 with the Chandra High Energy Transmission Grating Spectrometer (HETGS) within our HETG GTO time program for a total exposure time of 150ks, allowing for full coverage of almost eight binary orbits. This enables us to update the quadratic ephemeris of the orbit. We also confirm a previous suggestion that the observed photo-ionized line emission originates from a confined region in the outer edge of the accretion disk, likely the hot spot. This allows us to probe geometrical properties such as the size of the accretion disk and the ADC, and also obtain a phase-resolved ionization balance of the line emitting region.
Canizares Claude
Ji Liangliang
Noble Michael
Nowak Michael
Schulz Norbert
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