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

双 X 射线星 X 射线的长期时间变化。

• 批准号: 63540197
• 负责人: MIYAMOTO Sigenori
• 金额: $ 0.7万
• 依托单位: Osaka University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for General Scientific Research (C)
• 财政年份: 1988
• 资助国家: 日本
• 起止时间: 1988 至 1989
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-63540197/
• 关键词: X-ray star; X-ray nova; Compton scattering; Black hole; neutron star; X-ray radiation; Phase lag; Time lag; X線星; X線放射メカニズム; 逆コンプトン散乱; 宇宙X線塵散乱; ブラックホール; X線星モニター観測; X線星スピン周期変化

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.

利用GINGA上的全天监视器（ASM）和大面积计数器（LAC）观测了X射线双星的X射线时间变化。通过ASM，我们发现了超过13个所谓的X射线新星。其中有GS 2000 +25和GS 2023 +338，由于它们的时间变化和X射线的能量谱，它们似乎是黑洞的候选者。我们还研究了天鹅座X-1和GX 339 -4的X射线时间变化，它们也是黑洞候选者，我们于1989年4月26日发现了GS 2023 +25。它从出现到消失的整个行为与1989年5月21日发现的黑洞候选X射线星星AO 620 - 00. GS 2023 +338非常相似。该源显示出非常大的，短期和长期的时间变化，在6月1日之前高达约500倍。在此之后，这个源显示出快速的时间变化，这与天鹅座X-1在其低状态下的变化非常相似。用LAC对天鹅座X-1进行了观测，发现其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该源的能谱。我们还发现了两个特征时间常数，分别为0.2秒和0.7秒，利用这两个特征时间常数，我们可以再现该源X射线的功率密度谱和相位滞后结构。我们还用LAC观测了这个源，发现相位滞后结构可以用尺寸约为2 × 10^9cm的康普顿散射云的存在来解释。基于这一事实，我们提出了一个喷流模型，它可以解释这种源的能谱和相位滞后结构。

项目成果

H.Tsunemi: "Pulse periods and Long-term Variations of the X-ray Pulsars Vela X-1 and Centaurus X-3" Publications of the Astronomical Society of Japan. 41. 453-460 (1989)

H.Tsunemi：“X 射线脉冲星 Vela X-1 和 Centaurus X-3 的脉冲周期和长期变化”，日本天文学会出版物。

S. Kitamoto, H. Tsunemi, S. Miyamoto, K. Yamashita, S. Mizobuchi, M. Nakagawa, T. Dotani and F. Makino: "GS2023+338: a New Class of X-ray Transient source ?" Nature 342 518-520, 1989.

S. Kitamoto、H. Tsunemi、S. Miyamoto、K. Yamashita、S. Mizobuchi、M. Nakakawa、T. Dotani 和 F. Makino：“GS2023 338：新型 X 射线瞬态源？”

H. Tsunemi, S. Kitamoto, S. Okamura and D. Roussel-Dupre: "Discovery of a Bright X-ray Nova GS2000+25." Astrophysical Journal 337 L81-L84, 1989.

H. Tsunemi、S. Kitamoto、S. Okamura 和 D. Roussel-Dupre：“发现明亮的 X 射线新星 GS2000 25。”

S. Miyamoto and S. Kitamoto: "X-ray Time Variations from Cygnus X-1 and Implications for the Accretion Process." Nature 342 773-774, 1989.

S. Miyamoto 和 S. Kitamoto：“天鹅座 X-1 的 X 射线时间变化及其对吸积过程的影响。”

H.Tsunemi: "Puke periods and the Longーterm Variations of the Xーray pulsons vala Xー1 and Centansus Xー3" Publications of the Astronomical Society of Japan. 41. 453-460 (1989)

H.Tsunemi：“Puke periods and the Long-term Variations of the X-ray pulsons vala X-1 and Centansus X-3” Publications of the Astronomical Society of Japan 41. 453-460 (1989)。