跳到主要內容

臺灣博碩士論文加值系統

(3.95.131.146) 您好!臺灣時間:2021/07/29 00:55
字體大小: 字級放大   字級縮小   預設字形  
回查詢結果 :::

詳目顯示

: 
twitterline
研究生:黃修慧
研究生(外文):Hsiu-Hui Huang
論文名稱:Geminga的X射線脈衝分析
論文名稱(外文):Search for Pulsation Signatures in the X-ray Emission from Geminga
指導教授:張祥光張祥光引用關係
指導教授(外文):Hsiang-Kuang Chang
學位類別:碩士
校院名稱:國立清華大學
系所名稱:物理學系
學門:自然科學學門
學類:物理學類
論文種類:學術論文
論文出版年:2004
畢業學年度:92
語文別:英文
論文頁數:54
中文關鍵詞:Geminga波霎中子星X射線脈衝分析
外文關鍵詞:GemingaPulsarneutron starx-raytiming analysis
相關次數:
  • 被引用被引用:0
  • 點閱點閱:120
  • 評分評分:
  • 下載下載:10
  • 收藏至我的研究室書目清單書目收藏:0
Geminga 是一顆沒有無線電波輻射但在X射線(X-ray)和伽馬射線(γ-ray)波段有觀測到以週期0.237秒自轉的波霎(pulsar)。我們使用ASCA和XMM人造衛星取得的數據來分析Geminga 在X射線波段的週期性行為,而我們選定探討的週期範圍為0.1秒到100秒之間。在分析過程中,我們使用H-test和epoch folding方法,以每一個間格為五分之一的傅立葉寬度(Fourier width)進行搜尋。如果我們能找到不是自轉的週期,也許能暗示中子星星震的存在或是說中子星表面存在波的傳遞。經過我們對此週期範圍的徹底搜尋,並未發現任何證據能說明星震的存在。最後,依據不同的觀測資料,對可能存在於中子星表面的波而言,我們給出3 倍標準差信心水準的能量通量(flux)上限:由1994、1999年ASCA的資料,得到3.5×10^-14 erg/cm^2/sec和1.9×10^-14 erg/cm^2/sec,分別為原來星體能量通量的12.4﹪和6.9﹪。從2002年XMM的數據,我們對不同能量範圍求得7.7×10^-13 erg/cm^2/sec(0.2-0.7 keV)和1.7×10^-14 erg/cm^2/sec(0.7-5.0keV),分別為原來波霎能量通量的1.3﹪和3.3﹪。
Geminga is a radio-quiet, rotation-powered pulsar with a 237-msec period observed in X-ray and gamma-ray bands. We conduct a periodicity search with its ASCA data and XMM-Newton data in the period range of 0.1 sec to 100 sec. The H-test and the method of epoch folding are employed with period search steps at one fifth of the corresponding Fourier widths. Periods other than the already known pulsar period, if found, may indicate the phenomenon of neutron star oscillations, which in a broad sense include waves on the stellar surface. We have found no evidence for such oscillations in our search. Upper limits to the pulsed component of these possible oscillations at the 3-sigma level inferred from the 1994 and 1999 ASCA data in 0.7-5 keV are 3.5x10^-14 erg/cm^2/sec and 1.9x10^-14 erg/cm^2/sec respectively, which are 12.4\% and 6.9\% of the source flux. 3-sigma upper limits inferred from 2002 XMM-Newton data in energy bands of 0.2-0.7 and 0.7-5 keV are 7.7x10^-13 erg/cm^2/sec and 1.7x10^-14 erg/cm^2/sec, which are 1.3\% and 3.3\% of the source flux respectively.
1. Introduction
1.1 Motivation
1.2 Geminga---PSR J0633+1746
1.3 ASCA---The Advanced Satellite for Cosmology and Astrophysics
1.4 RXTE---The Rossi X-ray Time Explorer
1.5 XMM---The X-ray Multi-Mirror Observatory
2. Data Reduction
2.1 Observations
2.2 Reduction Procedures
2.2.1 ASCA Observation
2.2.2 RXTE Observation
2.2.3 XMM-Newton Observation
3. Data Analysis
3.1 Methods of Timing Analysis
3.1.1 Epoch Folding
3.1.2 The H-test
3.2 Analysis Procedures
4. Results and Discussion
4.1 Search for Other Periodicities
4.2 Discussion
5. Summary
Bertch, D. L. et al. 1992, Nature, 357, 306
Bignami, G. F., Caraveo, P. A., & Lamb, R. C. 1983, ApJ, 272, L9
Bignami, G. F., Caraveo, P. A., & Paul, J. A. 1988, A\&A, 202, L1
Bignami, G. F. et al. 1987, ApJ, 319, 358
Boriakoff, V. 1976, ApJ, 208, L43
Buccheri, R. et al. 1998, The Many Faces of Neutron stars, 525-537, Kluwer Academic Publishers.
Caraveo, P. A. et al. 1996, ApJ, 461, L91
Caraveo, P. A. et al. 2003, Science, 301, 1345
Caraveo, P. A. et al. 2004, Mem. S.A.It. Vol. 75, 470
Carroll, B. W. & Ostlie, D. A. 1996, An Introduction to Modern Astrophysics, Addison Wesley.
Cheng, K. S., Gil, J. & Zhang, L. 1998, ApJ, 493, L35
Cheng, K. S. & Zhang, L. 1999, ApJ, 515, 337
Chukwude, A. E. 2003, A&A, 406, 667
Cordes, J. M. & Greenstein, G. 1981, ApJ, 245, 1060
Crawford, F. & Demianski, M. 2003, ApJ, 595, 1052
De Jager, O.C. et al. 1989, A&A, 221,180
Dodson, R. G., McCulloch, P. M. & Lewis, D. R. 2002, ApJ, 564, L85
Fichtel, C. E. et al. 1975, ApJ, 198, 163
Goldreich, P. & Julian, W. H., 1969, ApJ, 157, 869
Halpern, J. P. & Holt, S. S., 1992, Nature, 357, 222
Halpern, J. P. & Ruderman, M., 1993, ApJ, 415, 286
Halpern, J. P. & Tytler, D. 1988, ApJ, 330, 201
Halpern, J. P. & Wang, F. Y.-H. 1997, ApJ, 477, 905
Hobbs, G. et al. 2002, Mon. Not. R. Astron. Soc. 333, L7
Jackson, M. S. et al. 2002, ApJ, 578, 935
Leahy, D. A. 1987, A&A, 180, 275
Lewis, David A., Methods of Experimental Physics, Vol. 28, 349
Lyne, A. G. & Graham-Smith, F. 1998, Pulsar Astronomy, Cambridge University Press.
Lyne, A. G., Shemar, S. L. & Graham-Smith, F. 2000, Mon. Not. R. Astron. Soc. 315, 534
Malofeev, V. M. & Malov, O. I. 1997, Nature, 389, 697
Mattox, J. R., Halpern, J. P., and Caraveo, P. A. 1998, ApJ, 493, 891
Rankin, J. M., 1986, ApJ, 301, 901
Ruderman, M. A. & Sutherland, P. G. 1975, ApJ. 196, 51
Ruderman, M. A. 1970, Nature, 225, 619
Scott, D. M., Finger, M. H., and Wilson, C. A. 2003, Mon. Not. R. Astron. Soc. 344, 412
Str?er, L. et al. 2001, A&A, 365, L18
Thompson, D. J. et al. 1977, ApJ, 213, 252
Turner, M. J. L. et al. 2001, A&A, 365, L27
Wang, F. Y.-H., Ruderman, M., Halpern, J. P. & Zhu, T. 1998, ApJ, 498, 373
Wasaburo Unno et al. 1989, Nonradial Oscillations of Stars, University of Tokyo Press.
QRCODE
 
 
 
 
 
                                                                                                                                                                                                                                                                                                                                                                                                               
第一頁 上一頁 下一頁 最後一頁 top