觀測黑洞X光瞬變源X1755-338在2020-2021的爆發｜國立清華大學博碩士論文庫

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研究生：	鄭佳榮 Cheng, Chia-Jung
論文名稱：	觀測黑洞X光瞬變源X1755-338在2020-2021的爆發 Observations of the black hole X-ray transient X1755-338 in the 2020-2021 outburst
指導教授：	江國興 Kong, K. H. Albert
口試委員:	張祥光 Chang, Hsiang-Kuang 胡欽評 Hu, Chin-Ping
學位類別：	碩士 Master
系所名稱：	理學院 - 物理學系 Department of Physics
論文出版年：	2021
畢業學年度：	109
語文別：	英文
論文頁數：	88
中文關鍵詞：	黑洞物理、雙星系統、吸積過程、黑洞X光瞬變源
外文關鍵詞：	Black hole physics, Binaries, Accretion, Black hole X-ray transient
相關次數：	點閱：3 下載：0
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低質量X光雙星系統是由一顆在中心的緻密星體(黑洞或中子星)經由洛希瓣吸積低質量伴星所組成。X光新星，又稱作軟X光瞬變源，是低質量X光雙星系統的一個分支，此系統長時間處在靜止態，偶然會轉變進入爆發的狀態，此時我們可以在X光、可見光波段偵測到它。在爆發態時，從內部吸積盤產生的X光射線在短時間內會大量增加，受到這些X光照射的外部吸積盤跟伴星會再產生可見光。觀測高傾角的低質量X光雙星系統可以幫助我們了解吸積盤上的物質分布與內容。此外，分析軟X光瞬變源在不同放射狀態下X光與可見光的訊號提供我們機會去說明吸積的過程與結構。
本論文主要目標是去探討正在爆發狀態的黑洞X光瞬變源X1755-338在2020-2021年的行為。黑洞X光瞬變源X1755-338有一個很有趣的特性，它在上一次爆發過程中(1984)，在X光與可見光波段被觀察到有4.46個小時的軌道週期。有鑑於此，我們在2020-2021利用鹿林天文台一公尺可見光望遠鏡去觀測X1755-338並嘗試獲得跟上一次接近的週期結果。出乎意料的是，4.46小時的週期在可見光與X光同時消失了，我們也發現一些證據指出這次的爆發明顯比上一次來得弱，這可能也意味著黑洞X光瞬變源X1755-338在這兩次的爆發中展現了不一樣的吸積過程與機制，這可能也是造成4.46小時週期消失的主要原因。
另外，我們也展示了在日本希望號實驗艙上全天X光射線監視裝置(MAXI)的每天平均X光曲線。除此之外，我們利用高能量X光曲線產生器去尋找所有觀測過黑洞X光瞬變源X1755-338的X光任務並展示從1969年到2021年長期的X光曲線。並且為了找出一些有關X1755-338長期變化與不尋常長時間爆發行為的線索，我們嘗試將X1755-338與另一個軟X光瞬變源GRS 1915+105做比較，儘管它們有相似的行為表現，但是本質上它們還是有許多的不同之處，加上我們對於X1755-338的距離與中心黑洞質量還存在很大的不確定性，要解釋其行為還需要更多精確的資訊。

Low-mass X-ray binaries (LMXBs) are binary systems where a black hole or a neutron star accretes from a low mass companion star through Roche-lobe overflow. X-ray novae, also known as soft X-ray transients (SXTs) is a subset of LMXBs. SXTs stay in quiescent state for a long time and accidentally turn into an outburst such that we can detect them in X-ray and optical bands. During an outburst, the X-ray flux of X-ray binary which originates from the inner accretion disk increases considerably and reprocesses in the outer accretion disk and the companion star to produce optical emission. Observing high inclination LMXBs during an outburst can help us to clarify the characteristics and distribution of the gas surrounding the X-ray-illuminated accretion disk. Furthermore, studying X-ray and optical emissions of SXTs at different emission states provides us an opportunity to explicate the accretion process and the geometry of the systems.
The primary objective of this thesis is to study a black hole X-ray binary currently in outburst. Our target, X1755-338, is a black hole X-ray binary with a 4.46-hr orbital period in both X-ray and optical bands. We use the Lulin One-Meter Telescope (LOT) to monitor the optical behaviors of X1755-338 in 2020 and 2021 and attempt to reproduce the 4.46-hr optical light curves. However, there is evidence that the current outburst is a failed (weaker) one and this indicates a slightly different accretion geometry compared with the last outburst.
In addition, we exhibit MAXI daily average light curves in order to obtain more information about this rare failed outburst. We also search all the historical X-ray missions and investigate the X-ray long-term light curve of X1755-338 from 1969-2021. Furthermore, in order to interpret the long-time scale variations and extraordinary long duration outburst, we compare X1755-338 with another SXTs, GRS 1915+105 which show similar long-term X-ray behaviors. We conclude that they are still quite different with the diverse observational and intrinsic physical properties.

摘要........................................................I
Abstract...................................................II
Acknowledgements...........................................IV
Contents...................................................VI
List of Figures............................................IX
List of Tables............................................XII
Chapter 1 Introduction......................................1
1    X-ray binaries.......................................1
1.1    High-mass X-ray binaries (HMXBs)...................2
1.2    Low-mass X-ray binaries (LMXBs)....................4
1.3    X-ray dippers......................................6
2    Black hole binaries (BHBs)...........................7
2.1    X-ray light curves and spectra of BHBs, BHCs......10
3    Emission states of BHBs.............................13
3.1    Quiescent state...................................13
3.2    High/Soft (HS) state..............................14
3.3    Low/Hard (LH) state...............................15
3.4    Steep power-law or Very High (VH) state...........17
3.5    Intermediate state................................19
4    X-ray novae.........................................20
5    Disk instability model..............................22
5.1    Advection-dominated accretion flow................23
6    Mechanisms for the outbursts of SXTs................25
Chapter 2 X1755-338........................................28
1    X1755-338 during the outbursts and the quiescence...30
2    X-ray dips and iron emission line...................31
3    Motivation and objectives of this work..............32
Chapter 3 Instrumentation..................................33
1    Lulin Observatory...................................33
2    MAXI................................................34
Chapter 4 Data Analysis....................................36
1    LOT Optical Observations............................36
1.1    Data Reduction and Alignment......................36
1.2    Point-Spread Function (PSF) Photometry............38
1.3    Differential Photometry and Periodogram...........41
1.4    SDSS g-band filter (410-552nm)....................41
1.5    SDSS r-band filter (550-694nm)....................42
1.6    SDSS i-band filter (694-847nm)....................43
1.7    Lomb-Scargle Periodogram..........................44
2    MAXI X-ray light curves of X1755-338................45
3    X-ray long-term light curve of X1755-338............46
Chapter 5 Results and Discussion...........................47
1    LOT Optical light curves of X1755-338...............47
1.1    LOT Optical light curves of each date.............47
1.2    Periodograms and folded light curves with 4.46-hr period...53
1.3    Summary...........................................57
2    MAXI X-ray light curves of X1755-338................58
2.1    Daily Average Light Curves of MAXI................58
3    X-ray long-term light curve of X1755-338............60
4    Discussion and Conclusion...........................63
4.1    Missing 4.46-hr Period............................63
4.2    HS state and unusual duration of the outburst.....65
Chapter 6 Summary and Future Works.........................72
1    Summary.............................................72
2    Future Works........................................73
Bibliography...............................................75
Appendix...................................................82

                                

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