Emission lines from X-ray-heated accretion disks in low-mass X-ray binaries

Details Emission lines from X-ray-heated accretion disks in low-mass X-ray binaries Emission lines from X-ray-heated accretion disks in low-mass X-ray binaries

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...431..273k&link_type=abstract

The Astrophysical Journal, Part 1, vol. 431, no. 1, p. 273-301

Mathematics

Probability

77

Accretion Disks, Emission Spectra, Line Spectra, Stellar Coronas, Stellar Mass Accretion, X Ray Binaries, Abundance, Astronomical Models, Compton Effect, Photoionization, Spectrum Analysis, Temperature Distribution, X Ray Spectra

Scientific paper

We investigate the structure of accretion disks illuminated by X-rays from a central compact object in a binary system. X-rays can photoionize the upper atmosphere of the disk and form an accretion disk corona (ADC) where emission lines can form. We construct a model to calculate the vertical structure and the emission spectrum of the ADC with parameters appropriate to low-mass X-ray binaries. These models are made by nonlocal thermodynamic equilibrium calculations of ion and level populations and include a large number of atomic processes for 10 cosmically abundant elements. Transfer of radiation is treated by using the escape probability formalism. The vertical temperature profile of the ADC consists of a Compton-heated region and a mid-T zone where the temperature is approximately 106 K. A thermal instability occurs close to the disk photosphere and causes the temperature of the ADC to drop abruptly from 106 K to several times 104 K. The emission spectrum in the optical, ultraviolet, extreme ultraviolet, and X-ray range is discussed and compared with the observations.

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