以X射線連續光譜限制在GX 339-4中的黑洞的自旋

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姓名

蘇羿豪(Yi-Hao Su) 查詢紙本館藏

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天文研究所

論文名稱

以X射線連續光譜限制在GX 339-4中的黑洞的自旋
(Constraint on the Spin of the Black Hole in GX 339-4 from X-ray Continuum)

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摘要(中)

我們利用擬合X 射線連續光譜方法去限制 X 射線雙星GX 339-4 中的恆星級黑洞的自旋。Reis et al. (2008) 利用鐵K α 線模型測定出它的自旋為a*=0.935±0.01。然而，Kolehmainen & Done (2010)從X 射線連續光譜中得到它的自旋不會超過0.9 的結果。為了解決這兩個不一致的結果並計算其自旋，我們先採用兩個相對論性吸積薄盤模型，並且結合簡單的康普吞化模型，用以擬合RXTE/PCA 對於GX 339-4 自2002 年至2010 年的爆發觀測的X 射線連續光譜。我們依循McClintock et al. (2006) and Steiner et al. (2009a & 2010)的建議，為了利於進一步分析而設立了限制條件以挑選符合吸積薄盤模型的資料。我們更進一步地利用新建立的修正模型(McClintock et al. 2006)去限制這黑洞的自旋。我們的結果顯示這個黑洞的自旋不會超過a*=0.94，這似乎支持了Reis et al. (2008)的結果。

摘要(英)

We present our analysis result for constraining the spin of the stellar-mass black hole (BH) in the X-ray binary GX 339-4 by fitting its X-ray continuum spectra. Reis et al. (2008) determined its spin to be a*=0.935±0.01 by modeling the profile of Fe K α line. However, Kolehmainen & Done (2010) concluded that its spin is no more than 0.9 from X-ray continuum fitting method. To resolve these contradictive results and estimate its spin, we first adopted two fully relativistic, thin accretion disk models
combined with a simple comptonization model to fit X-ray continuum spectra of GX 339-4 observed by Proportional Counter Array (PCA) on Rossi X-Ray Timing Explorer(RXTE) during its 2002-2010 outbursts. We set up constraints suggested by McClintock et al. (2006) and Steiner et al. (2009a & 2010) to select the data suitable for thin accretion disk model to further analyze. We then used the most recently developed modified model (McClintock et al. 2006) to further constrain the black hole spin. Our result indicates that the BH spin is no less than a*=0.94, which is likely favorable to the result from Reis et al. (2008).

關鍵字(中)

★ 吸積
★ X射線
★ 自旋
★ 黑洞

關鍵字(英)

★ black hole
★ spin
★ X-ray
★ accretion

論文目次

Contents-------------------------------------- i
List of Figures------------------------------- ii
List of Tables------------------------------- iii
Chapter 1 Introduction ....................... 1
1.1 Black Hole X-ray binaries ................ 1
1.1.1 States in Black Hole X-ray Binaries .... 2
1.1.2 X-ray Spectra .......................... 4
1.2 Measuring the Black Hole Spin ............ 6
1.3 GX 339-4 ................................. 8
1.4 Outline of This Thesis ................... 8
Chapter 2 Observation and Data Reduction ..... 9
2.1 RXTE .................................... 10
2.2 Observational Data Selection ............ 13
2.3 Data Reduction........................... 15
2.3.1 Software .............................. 15
2.3.2 Event Filtering and Data Reduction .... 16
Chapter 3 Data Anaysis ...................... 19
3.1 The Spectral models for Constraining the Black Hole Spin ....... 20
3.2 The Parameter Sets to Constrain the Black Hole Spin ....... 23
3.2.1 The Assumptions of Kolehmainen & Done (2010) ...23
3.2.2 The More Reasonable Parameter ................. 24
3.3 Constrain on the Spin by the Modified Spectral Model: KERRBB2 .... 27
Chapter 4 Discussion and Conclusion ................. 33
4.1 The Comparisons of Our Results with Previous Study .......33
4.2 The Spin Range of the Black Hole in GX 339-4........... 34
References .......................................... 36
Appendix ............................................ 39

參考文獻

1.Bardeen J. M., Press W. H., Teukolsky S. A., 1972, ApJ, 178, 347
2.Belloni T., Homan J., Casella P., van der Klis M., Nespoli E., Lewin W. H.G., Miller
3.J. M., Méndez M., 2005, A&A, 440, 207
Coriat M., Corbel S., Buxton M. M., Bailyn C. D., Tomsick 4.J. A., Körding E.,Kalemci E., 2009, MNRAS, 400, 123
5.Davis S. W., Blaes O. M., Hubeny I., Turner N. J., 2005, ApJ, 621, 372 (D05)
6.Davis, S. W., & Hubeny, I. 2006, ApJS, 164, 530
7.Esin A. A., McClintock J. E., Narayan R., 1997, ApJ, 489, 865
8.Fragos T., Tremmel M., Rantsiou E., Belczynski K., 2010, ApJ, 719, L79
9.Gallo, E., Fender, R., & Corbel, S. 2003, ATel, 196
10.Gallo, E., Corbel, S., Fender, R. P., Maccarone, T. J., & Tzioumis, A. K. 2004,MNRAS, 347, L52
11.Gilfanov,M. 2010, in Lecture Notes in Physics, Vol. 794, The Jet Paradigm, ed.T. Belloni (Berlin: Springer), 17
12.Harlaftis, E. T., & Greiner, J. 2004, A&A, 414, L13
13.Hynes, R. I., Steeghs, D., Casares, J., Charles, P. A., & O’Brien, K. 2003, ApJ,583, L95
14.Hynes, R. I., Steeghs, D., Casares, J., Charles, P. A., & O’Brien, K. 2004, ApJ,609, 317
15.Jahoda, K., Markwardt, C. B., Radeva, Y., Rots, A. H., Stark, M. J., Swank, J.H., Strohmayer, T. E., & Zhang, W. 2006, ApJS, 163, 401
16.Kalemci, E., et al. 2007, ATel, 1074
17.Kato, S., Fukue, J.,&Mineshige, S. 2008, Black-Hole Accretion Disks, Towards a New Paradigm (Kyoto: Kyoto Univ. Press)
18.King, A. R., Pringle, J. E., & Livio, M. 2007, MNRAS, 376, 1740
19.Kolehmainen, M., & Done, C. 2010, MNRAS, 406, 2206 (KD10)
20.Li, L.-X., Zimmerman, E. R., Narayan, R., & McClintock, J. E. 2005, ApJS,157, 335(L05)
21.McClintock, J. E., Shafee, R., Narayan, R., Remillard, R. A., Davis, S. W., & Li, L.-X.2006, ApJ, 652, 518
22.Miller, J. M., et al. 2004, ApJ, 606, L131
23.Miller, J. M. 2007, ARA&A, 45, 441
24.Miller, J. M., et al. 2009, ApJ, 697, 900
25.Miyakawa, T., Yamaoka, K., Homan, J., Saito, K., Dotani, T., Yoshida, A., &Inoue, H. 2008, PASJ, 60, 637
26.Muñoz-Darias, T., Casares, J., & Martínez-Pais, I. G. 2008, MNRAS, 385, 2205
27.Narayan, R., & Yi, I. 1994, ApJ, 428, L13
28.Narayan, R., & Yi, I. 1995, ApJ, 444, 231
29.Narayan, R. 1996, ApJ, 462, 136
30.Penna, R. F., McKinney, J. C., Narayan, R., Tchekhovskoy, A., Shafee, R., & McClintock, J. E. 2010, MNRAS, 408, 752
31.Reis, R. C., Fabian, A. C., Ross, R. R., Miniutti, G., Miller, J. M., & Reynolds,C. 2008, MNRAS, 387, 1489 (R08)
32.Remillard, R. A., & McClintock, J. E. 2006, ARA&A, 44, 49
33.Shakura, N. I., & Sunyaev, R. A. 1973, A&A, 24, 337
34.Smith D. M., Swank J. H., Heindl W. A., Remillard R. A., 2002, ATel, 85
35.Smith D. M., Heindl W. A., Swank J. H., Wilms J., Pottschmidt K., 2004,ATel, 231
36.Steiner, J. F., McClintock, J. E., Remillard, R. A., Narayan, R., & Gou, L. J.2009a, ApJ, 701, L83
37.Steiner, J. F., Narayan, R., McClintock, J. E., & Ebisawa, K. 2009b, PASP, 121,1279
38.Steiner, J. F., McClintock, J. E., Remillard, R. A., Gou, L. J., Yamada, S., &Narayan, R. 2010, ApJ, 718, L117
39.Swank, J. H., Smith, E. A., Smith, D. M., & Markwardt, C. B. 2006, ATel, 944, 1
40.Tananbaum, H., Gursky, H., Kellogg, E., Giacconi, R., & Jones, C. 1972, ApJ,177, L5
41.Tomsick, J. A. 2010, ATel, 2384, 1
42.Zdziarski, A. A.,Gierliński,M., Mikołajewska, J.,Wardziński, G., Smith,D.M.,Harmon, B. A., & Kitamoto, S. 2004, MNRAS, 351, 791

指導教授

周翊(Yi Chou)

審核日期

2011-7-14

推文