类星体PKS 1510-089的X射线流量变化周期特性

李孝攀; 张皓晶; 张雄

doi:10.7498/aps.60.089801

摘要

使用罗西X射线时变探测器的数据,得到了类星体PKS 1510-089从1996年1月到2009年12月在X射线的1.512 keV能段上的光变曲线.运用离散相关函数方法、小波分析方法和功率谱方法分析和认证类星体PKS 1510-089的光变周期值,结果表明类星体PKS 1510-089 在X射线的1.512 keV能段具有(0.940.08)a的平均光变周期.采用不同模型对观测到的周期性光变进行分析后的结果表明,超大质量双黑洞模型是目前解释类星体PKS 1510-089周期性光变较为理想的模型,应用

关键词:

Abstract

We present the X-ray light curve (1.512 keV) for quasar PKS 1510-089 with the observation of the all-sky monitor on the Rossi X-ray Timing Explorer from January 1996 to December 2009. Using the discrete correlation function method, the wavelet analysis method and the power spectrum method to analyze the data, we find that the light curve variability period of quasar PKS 1510-089 is (0.940.08)a. The super massive binary black hole model in used to analyze this source, and the results show that the orbit period of the super massive binary black hole system is (1.850.10)a and the super massive binary black hole model is the better model for describing the light curve periodic behaviour of quasar PKS 1510-089 at present.

Keywords:

作者及机构信息

1.
云南师范大学物理与电子信息学院,昆明 650092;

2.
昭通师范高等专科学校物理系, 昭通 657000

基金项目: 国家自然科学基金(批准号:10763002)和云南省自然科学基金重点项目 (批准号:2008A011Z)资助的课题.

Authors and contacts

1.
College of Physics and Electronics, Yunnan Normal University, Kunming 650092, China;

2.
Department of Physics, Zhaotong Teacher's School, Zhaotong 657000, China

参考文献

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施引文献

[1]	Kataoka J, Madejski G, Sikora M, Roming P, Chester M M, Grupe D, Tsubuku Y, Sato R, Kawai N, Tosti G, Impiombato D, Kovalev Y Y, Kovalev Y A, Edwards P G, Wagner S J, Moderski R, Stawarz L, Takahashi T, Watanabe S 2008 Astrophys. J. 672 787
[2]	Marscher A P, Jorstad S G, Larionov V M, Aller M F, Aller H D, Lhteenmki A, Agudo Ivn, Smith P S, Gurwell M, Hagen-Thorn V A, Konstantinova T S, Larionova E G, Larionova L V, Melnichuk D A, Blinov D A, Kopatskaya E N, Troitsky I S, Tornikoski M, Hovatta T, Schmidt G D, DArcangelo F D, Bhattarai D, Taylor B, Olmstead A R, Manne-Nicholas E, Roca-Sogorb M, Gmez Jos L, McHardy I M, Kurtanidze O, Nikolashvili M G, Kimeridze G N, Sigua L A 2010 Astrophys. J. 710 126
[3]
[4]
[5]	Xie G Z, Zhou S B, Li H T, Dai H, Chen L E, Ma L 2004 Mon. Not. Roy. Astron. Soc. 348 831
[6]	Daniel C, John F, Chi C, David H, Joanne M 2002 Astrophys. J. 580 742
[7]
[8]
[9]	Singh K P, Shrader C R, George I M 1997 Astrophys. J. 491 515
[10]
[11]	Wu J, Zhou X, Peng H, Ma J, Jiang Z, Chen J 2005 Mon. Not. Roy. Astron. Soc. 361 155
[12]	Li J, Fan J H, Yuan Y H 2007 Chin. Phys. 16 876
[13]
[14]	Pucella G, Vittorini V, DAmmando F, Tavani M, Raiteri C M, Villata M, Argan A, Barbiellini G, Boffelli F, Bulgarelli A, Caraveo P, Cattaneo P W, Chen A W, Cocco V, Costa E, Del Monte E, de Paris G, Di C G, Donnarumma I, Evangelista Y, Feroci M, Fiorini M, Froysland T, Fuschino F, Galli M, Gianotti F, Giuliani A, Labanti C, Lapshov I, Lazzarotto F, Lipari P, Longo F, Marisaldi M, Mereghetti S, Morselli A, Pacciani L, Pellizzoni A, Perotti F, Picozza P, Prest M, Rapisarda M, Rappoldi A, Soffitta P, Trifoglio M, Trois A, Vallazza E, Vercellone S, Zambra A, Zanello D, Antonelli L A, Colafrancesco S, Cutini S, Gasparrini D, Giommi P, Pittori C, Verrecchia F, Salotti L, Aller M F, Aller H D, Carosati D, Larionov V M, Ligustri R 2008 Astron. Astrophys. 491 21
[15]
[16]	Zhang H J, Zhao G, Zhang X, Dong F T, Xie Z H, Yi T F, Zheng Y G, Bao Y Y 2009 Sci. China G 52 1442
[17]
[18]
[19]	Liller M H H, Liller W 1975 Astrophys. J. 199 133
[20]	Villata M, Raiteri C M, Ghisellini G, De Francesco G, Bosio S 1997 Astron. Astrophys. Suppl. 121 119
[21]
[22]
[23]	Dai B Z, Xie G Z, Li K H, Zhou S B, Liu W W, Jiang Z J 2001 Astron. J. 122 290
[24]	Xie G Z, Yi T F, Li H T, Zhou S B, Chen L E 2008 Astron. J. 135 2212
[25]
[26]
[27]	Marek G, Jo N 2006 Mon. Not. Roy. Astron. Soc. 370 837
[28]	Rani B, Wiita P J, Gupta A C 2009 Astrophys. J. 696 2170
[29]
[30]
[31]	Levine A M, Morgan E H, Remillard R 2005 Am. Astrophys. Soc. 207 7204
[32]
[33]	Cheng Y, Zhang X, Wu L, Mao W M, You L S 2006 Acta Phys. Sin. 55 988 (in Chinese) [程勇、张雄、伍林、毛慰明、尤丽莎 2006 55 988]
[34]
[35]	Zhang H J, Zhao G, Zhang X 2010 Sci. China G 53 252
[36]
[37]	Yuan L 2008 Chin. Phys. B 17 170
[38]
[39]	Hovatta T, Lehto H J, Tornikoski M 2008 Astron. Astrophys. 488 897
[40]	Dong F T, Zhang X 2009 Acta Phys. Sin. 58 8116 (in Chinese) [董富通、张雄 2009 58 8116]
[41]
[42]	Mallat S G 1999 A Wavelet Tour of Signal Processing (New York: Academic Press) pp22101
[43]
[44]
[45]	Meyers S D, Kelly B G, Brien J J O 1993 Mon.Wen.Rev. 121 2858
[46]	Collineau S, Brunet Y 1993 Bound-layer Meteor. 65 357
[47]
[48]	Ishibashi W, Courvoisier T J 2010 Astron. Astrophys. 512 58
[49]
[50]	Zhang H J, Zhao G, Zhang X, Wang X H 2009 Astron. Soc. Pac. Conf. Ser. 408 388
[51]
[52]
[53]	Zhang H J, Zhang X 2007 Acta Phys. Sin. 56 4305 (in Chinese) [张皓晶、张雄 2007 56 4305]
[54]
[55]	Begelman M C, Blandford R D, Rees M J 1980 Nature 287 307
[56]	Homan D C, Ojha R, Wardle J F C, Roberts D H, Aller M F, Aller H D, Hughes P A 2001 Astron. J. 549 840
[57]
[58]	Jorstad S G, Marscher A P, Mattox J R, Wehrle A E, Bloom S D, Yurchenko A V 2001 Astrophys. J. Suppl. Ser. 134 181
[59]
[60]	Ghisellini G, Maraschi L, Treves A, Tanzi E G 1986 Astrophys. J. 310 317
[61]
[62]
[63]	Zhou S B 2004 Ph. D. Dissertation (Kunming:Yunnan Astronomical Observatory, Chinese Academy of Sciences) (in Chinese) [周曙白 2004 博士学位论文(昆明: 中国科学院云南天文台)]
[64]
[65]	Wallinder F H, Kato S, Abramowicz M A 1992 Astron. Astrophys. Rev. 4 79
[66]	Jiao C L, Xue L, Gu W M, Lu J F 2009 Astrophys. J. 693 670
[67]
[68]
[69]	Zhang X, Zheng Y G, Zhang H J, Hu S M, Xie Z H 2006 Chin. Phys. 15 2185

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