長久以來，黑洞一直是宇宙中最神祕且迷人的天體，但我們對它的知識依舊十分有限。黑洞吸收了所有光線，於是我們難以直接觀測，但若是它身邊有一顆伴星（恆星），兩個天體會因為重力束縛而形成一個互繞旋轉的系統，並藉由物質吸積過程放出X射線，這就是黑洞雙星系統（Black Hole Binary,BHB）。我們通常可以趁著X射線爆發（X-ray outburst）的時候觀測到它們，因為這類星體大部分時間光度非常暗，而X射線爆發期間，每秒最多可以收集超過2000顆高能光子，這樣的資料量讓我們得以進行合理的討論與分析。關於系統突然發亮背後的原因，最廣泛被接受的說法是歸因於吸積率的變化，而這正是篇論文想要探討的題目。這篇論文針對兩個黑洞雙星系統來探討發生outburst期間，光譜及時域特性的變化，藉此推斷系統的吸積過程。

第一個系統名為MAXI J1535-571，是一顆新發現的銀河系內黑洞雙星系統。它在2017/09/02第一次被偵測到，即是因為系統產生了X-ray outburst。我們於是分析了橫跨爆發前期約50天的公開觀測資料（09/04-10/24，MJD 58000{58050），來研究這顆新天體。這些資料分別來自架設於兩座衛星上的三個太空望遠鏡，Swift/XRT (0.5-10 keV)、Swift/BAT (15-60 keV)以及MAXI/GSC (7-20keV)。我們利用描述現象的數學模型（pow-law、黑體輻射模型）來分析光譜，並以高能/低能光子的比例（hardness ratio）決定光譜型，結合時域分析方法所得到的準週期振盪（Quasi-Periodic Oscillation）結果，來判斷爆發期間的吸積進程演化。

另一個系統名為V404 Cygni，是一顆非常有名的系內黑洞雙星系統。它結束了26年的寂靜狀態後，再一次被偵測到X射線爆發，且因為亮度變化非常劇烈且毫無規律，完全不像以往觀測到的爆發表現，使得天文學家們對這顆天體產生極大興趣。我們收集了Swift衛星搭載的兩個太空望遠鏡所觀測的公開資料，以及INTEGRAL/IBIS太空望遠鏡的偏振觀測資料，針對爆發最活躍的幾天進行詳細的分析，試圖在短時間尺度下討論光譜型、時域特性和偏振變化之間的關係是否有跡可循。

Black holes are certainly one of the most stunning objects in the Universe. Our knowledge of black holes, however, is still very limited. We cannot see them since there is no light coming directly from a black hole, but they do send us messages through some ways when they have a companion star. They are black hole binaries (BHBs). BHBs in our Galaxy are usually discovered as X-ray transients when an outburst occurs. During the outburst, high X-ray flux provides astronomers an observing window to carry out feasible studies of BHBs. In this thesis, studies for two BHBs, MAXI J1535 571 and V404 Cygni, in the high-energy regime will be presented.
The Galactic X-ray transient MAXI J1535 571 was monitored extensively in multi-wavelength during its outburst immediately after its discovery on 2017 September 2. We studied this source in detail during the initial period (from 2017 September 4 to October 24; MJD 58000 to 58050). The combined spectra of Swift/XRT (0.5–10 keV), Swift/BAT (15–60 keV) and MAXI/GSC (7–20 keV) were studied with phenomenological models, and XRT light curves were used for studying the quasi-periodic oscillation (QPO) and time-lags phenomena. The evolution of the spectral state was derived based on temporal and spectral properties, and physical explanations were discussed as well with the Two Component Advective Flow (TCAF) model.
V404 Cygni is a well-known black hole system located in constellation Cygnus. After 26 years of quiescence since its first X-ray discovery, it underwent another huge X-ray outburst in 2015 June. With many fierce X-ray bursts observed in a few days, its X-ray flux changed rapidly without a clear pattern. During flaring, the maximum X-ray flux reached ⇠50 Crab, which made it the brightest X-ray source in the sky at the time. The X-ray spectra of V404 Cygni also showed strong variability on a very short time-scale during the outburst, and that is not typical for BHBs. We studied its spectral and temporal evolution with the TCAF model and extensively investigated its polarization phenomena in soft gamma-rays using the newest INTEGRAL/IBIS data and the corresponding analysis pipeline.

1 Introduction
1.1 OutburstofBlackHoleBinaries(BHBs) ................. 1
1.1.1 AccretionDynamicsandSpectralStates . . . . . . . . . . . . . 2
1.1.2 Quasi-PeriodicOscillation ..................... 3
1.2 SwiftandMAXI .............................. 6
1.2.1 The Neil Gehrels Swift Observatory (Swift) . . . . . . . . . . . 6
1.2.2 TheMonitorofAll-skyX-rayImage(MAXI) . . . . . . . . . . 9
1.3 INTEGRAL/IBIS.............................. 11
1.3.1 PolarizationMeasurement ..................... 14

2 Studying X-ray Outburst of BHB Using The TCAF Model
2.1 The Two Component Advective Flow (TCAF) Solution . . . . . . . . . 17
2.1.1 ImplementationinXSPEC..................... 18
2.2 CaseStudy ................................. 20
2.2.1 The2017OutburstOfMAXIJ1535 571 . . . . . . . . . . . . . 20
2.2.2 The2015OutburstOfV404Cygni ................ 21

3 MAXI J1535 571
3.1 ObservationsandDataReduction..................... 23
3.2 Results.................................... 25
3.2.1 TimingAnalysis........................... 27
3.2.2 PhenomenologicalSpectralModelling . . . . . . . . . . . . . . . 30
3.2.3 TimeLagStudy........................... 31

4 V404 Cygni
4.1 SpectroscopywithTCAFModel...................... 40
4.2 PolarizationStudyUsingINTEGRAL/IBIS . . . . . . . . . . . . . . . 47
4.2.1 Modulationfitting ......................... 48

5 Discussion and Conclusion
5.1 MAXIJ1535 571.............................. 57
5.1.1 SpectralStateEvolution ...................... 57
5.1.2 LFQPOsandTheStandingShock................. 60
5.2 V404Cygni ................................. 61
5.2.1 TCAFFitting............................ 61
5.2.2 Polarization............................. 62
5.3 ConcludingRemark............................. 63
bibliography............................. 65

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