BL Lac天体1ES 1959+650的长周期光变研究
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摘要
根据芬兰Tuorla天文台的光学观测数据,采用功率谱方法、DCF(Discrete Correlation Function)方法和Jurkevich 3种方法,获得BL Lac星系1ES 1959+650的长期光变周期是P=1.4±0.3 yr.假定该周期来源与吸积盘有关,可以得到该源的不稳定性发生的区域是R=9.65R_g(R_g是席瓦西半径).
In this paper,the long-term observations of Tuorla Observatory in Finland are collected.The power spectrum,the DCF(Discrete Correlation Function) method,and the Jurkevich method are used to analyze the periodicity.The results show that the periodicity of BL Lac Object 1ES 1959+650 is P=1.4±0.3 yr.Considering that there is a relation between the origin of periodicity and accretion disk,we use this periodicity to obtain the unstable region lying at R=9.65R_g,where R_g represents the Schwarzschild radius.
In this paper,the long-term observations of Tuorla Observatory in Finland are collected.The power spectrum,the DCF(Discrete Correlation Function) method,and the Jurkevich method are used to analyze the periodicity.The results show that the periodicity of BL Lac Object 1ES 1959+650 is P=1.4±0.3 yr.Considering that there is a relation between the origin of periodicity and accretion disk,we use this periodicity to obtain the unstable region lying at R=9.65R_g,where R_g represents the Schwarzschild radius.
引文
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[2]Gupta A C,Banerjee D P K,Ashok N M,et al.A&A,2004,422:505
[3]Burbidge G R,Jones T W.ApJ,1974,193:43
[4]Wagner S J,Witzel A.ARA&A,1995,33:163
[5]Kunkel W E.AJ,1967,72:1341
[6]Raiteri C M,Vallata M,Aller H D,et al.A&A,2001,377:396
[7]Elvis M,Plummer D,Schachter J,et al.ApJS,1992,80:257
[8]Schachter J F,Stocke J T,Perlman E,et al.ApJ,1993,412:541
[9]Heidt J,Nilsson K,Sillanp(a|¨)(a|¨)A,et al.A&A,1999,341:683
[10]Hartman R C,Bertsch D L,Bloom S D,et al.ApJS,1999,123:79
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[12]Deeming T J.Ap&SS,1975,36:137
[13]Lomb N R.Ap&SS,1976,39:447
[14]Edelson R A,Krolik J H.ApJ,1988,333:646
[15]Hufnagel B R,Bregman J N.ApJ,1992,386:473
[16]Fan J H.ChJAS,2005,5:213
[17]Jurkevich I,Usher P D,Shen B S P.Ap&SS,1971,10:402
[18]Kidger M,Takalo L,Sillanpaa A.A&A,1992,264:32
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[22]Falomo R,Kotilainen J K,Treves A.ApJ,2002,569:35