A Long term time variation of the X-rays from binary X-ray stars.

用Ginga上的全天监视器(ASM)和大面积计数器(LAC)观测了来自双星X射线的X射线的时间变化。通过ASM，我们发现了超过13个所谓的X射线新星。其中有GS2000+25和GS2023+338，由于它们的时间变化和X射线能谱，它们似乎是黑洞候选者。我们还研究了同样是黑洞候选者的天鹅座X-1和GX339-4的X射线时间变化，我们在1989年4月26日发现了GS2023+25。它从出现到消失的整个行为与黑洞候选X射线星AO620-00非常相似。GS2023+338于1989年5月21日被发现。该震源在6月1日前表现出很大的、短期的和长期的时间变化，最高可达500倍左右。在此之后，该源表现出快速的时间变化，这与天鹅座X-1在其低状态下的变化非常相似。天鹅座X-1的时间变化的功率密度谱和滞后时间结构与天鹅座X-1的相似，发现天鹅座X-1的时间变化的滞后结构不能用康普顿散射模型来解释，而康普顿散射模型被认为可以解释这一源的能谱。我们还发现了约0.2秒和0.7秒的两个特征时间常数，可以用来再现来自该源的X射线的功率密度谱和位相滞后结构。我们还用LAC观测了这一源，发现这种位相滞后结构可以用大小约2×10~(-9)cm的康普顿散射云的存在来解释。基于这一事实，我们提出了一个可以解释这一源的能谱和相位滞后结构的喷流模型。

Time variation of X-rays from binary X-ray stars are observed with the all sky monitor, (ASM) and the large area counters (LAC) onboard GINGA. With ASM we found more than 13 so-called X-ray novas. Among these, there are GS2000+25 and GS2023+338, which seem to be black hole candidates because of their time variations and energy spectra of X-rays. We also studied the X-ray time variations of Cygnus X-1 and GX339-4, which were also black hole candidates.We discovered GS2023+25 on 26th April 1989. Its whole behavior from the appearance to the disappearance was very similar to the black hole candidate X- ray star AO620-00.GS2023+338 was discovered on 21st May 1989. This source showed very large, short and long term time variations up to the factor of about 500 before 1st of June. After this time, this source showed rapid time variations which was very similar to those of Cygnus X-1 in its low state. The power density spectrum and the lag time structure of its time variations were similar to those of Cygnus X-1.Cygnus X-1 was observed with LAC, and we found the structure of the time lag of the time variations can not be explained by the Compton scattering model, which had been assumed to explain the energy spectrum of this source. We also found there were two characteristic time constants of about 0.2 sec and 0.7 sec, with which we could reproduce the power density spectrum and phase lag structure of X-rays from this source.We found there existed very high state in GX339-4 from the observation with ASM. We also observed this source with LAC and found the phase lag structure could be explained by the existence of the Compton scattering cloud of the size of about 2 10^9cm. Based on this fact we proposed a jet model which can explain the energy spectrum and the phase lag structure of this source.