SIMBAD references

Understanding the properties of the hot corona is important for studying the accretion disks in black hole X-ray binary systems. Using the Monte Carlo technique to simulate the inverse Compton scattering between photons emitted from the cold disk and electrons in the hot corona, we have produced two table models in the XSPEC format for the spherical corona case and the disklike (slab) corona case. All parameters in our table models are physical properties of the system and can be derived from data fitting directly. Applying the models to broadband spectra of the black hole candidate XTE J2012+381 observed with BeppoSAX, we estimate the size of the corona and the inner radius of the disk. The size of the corona in this system is several tens of gravitational radii, and the substantial increase of the inner disk radius during the transit from the hard state to the soft state is not found.