Optical Spectroscopic Observations of Cyg X-1=HDE 226868

We present the results of the spectroscopic observations of HDE 226868, the optical counterpart to the black hole X-ray binary Cyg X-1, from 2001 to 2006. We analyze the variabilities of the two components in the complex H$alpha$ line: one P-Cygni shaped component which follows the motion of the supergiant and another emission component moving with an antiphase orbital motion relative to the supergiant, which is attributed to a focused-stellar wind. The results of KOREL disentangling of our spectra indicate that the focused stellar wind is responsible for the major part of the variability of the H$alpha$ emission line. The emission of the supergiant component had a small difference between the low/hard and high/soft states, while the focused wind component became strong in the low/hard state and weak in the high/soft state. The wind is nearly undisturbed by the X-ray photoionization during the low/hard state. However, during the high/soft state, the X-rays from the compact object could decelerate the line-driven wind and result in a high mass accretion rate, due to the effect of the X-ray photoionization. The X-ray illuminating could also change the temperature profile of the stellar wind and increase its temperature, and thus decrease the H$alpha$ emissivity of the wind, which could explain the H$alpha$ variabilities of Cyg X-1 during different X-ray states.

Optical Spectroscopic Observations of CI Camelopardalis

We present the results of optical spectroscopic observations of CI Cam. Double-peaked profiles were simultaneously observed for the first time in the hydrogen Balmer, He {small I} $lambda$6678 and Fe {small II} lines during an observational run in 2001 September. An intermediate viewing angle of the circumstellar disk around the B[e] star is consistent with our data. A significant decrease in the intensity of the H$alpha$ and He {small I} lines in our 2004 September observations might have been the precursor of a line outburst at the end of 2004. The remarkable increase in the intensity of all lines and the decrease in visual brightness in 2005 might be due to the environment filling with new material ejected during the outburst. The environment of CI Cam is influenced by mass loss from the B[e] star and the outburst of its compact companion.