Optical And UV Light Curves Of The ADC Source 4U 1822-371

Details Optical And UV Light Curves Of The ADC Source 4U 1822-371 Optical And UV Light Curves Of The ADC Source 4U 1822-371

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.0311b&link_type=abstract

American Astronomical Society, AAS Meeting #211, #03.11; Bulletin of the American Astronomical Society, Vol. 39, p.724

Astronomy and Astrophysics

Astronomy

Scientific paper

The low-mass X-ray binary (LMXB) 4U1822-371 is the prototypical accretion disk corona (ADC) system. The ADC is a hard X-ray emitting region above and below the accretion disk, centered on the neutron star. It is believed that there is an ADC in most, if not all, LMXBs, but the ADC is faint and is not seen in most systems because the neutron star and inner disk are much brighter. The ADC is visible when the orbital inclination is high enough that the outer accretion disk blocks light from the neutron star and inner disk.
We have obtained new time-resolved UV spectrograms with the ACS/SBC on the Hubble Space Telescope and new V and J band light curves with the 1.3-m SMARTS telescope at CTIO. We present an updated optical/UV ephemeris for the times of eclipse. From our modeling of the UV light curves, we show that the ADC is a major source of the UV flux.

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