The low-mass X-ray binary (LMXB) 4U 1822-371 has an accretion disk corona (ADC) that scatters X-ray photons from the inner disk and neutron star out of the line of sight. It has a high orbital inclination and the secondary star eclipses the disk and ADC. We have obtained new time-resolved UV spectrograms and V- and J-band photometry of 4U 1822-371. The large quadratic term in our new optical eclipse ephemeris confirms that the system has an extremely high rate of mass transfer and mass accretion. The CIV λλ=1548-1550Å emission line has a half width of ∼4400 km/s, indicating a strong, high velocity wind is being driven off the accretion disk. Near the disk the wind is optically thick in UV, V, and J and the eclipse analysis shows that in V and J the optically thick wind extends nearly to the outer edge of the disk. The ADC must also extend vertically to a height equal to approximately half the disk radius. © 2010 American Institute of Physics.
Publication Source (Journal or Book title)
AIP Conference Proceedings
Bayless, A., Robinson, E., Hynes, R., Ashcraft, T., & Cornell, M. (2010). The structure of the accretion disk in the ADC source 4U 1822-371. AIP Conference Proceedings, 1248, 141-142. https://doi.org/10.1063/1.3475169