基于谱分析的Blazar天体光变周期研究
|
摘要
活动星系核AGNs (Active Galactic Nucleus)是中心区域有大能量辐射的一类特殊的星系。活动星系核的一些重要性质包括：它们具有恒星状的外表,随时间变化的连续光谱,以及宽的发射线等等。光变是活动星系核的普遍现象,从射电到X射线的所有波段都观测到了活动星系核的光变。光变对活动星系核中心区域的物理机制和理论模型作了有力的限定。
Blazar天体是射电噪AGNs,在所有的AGNs中光变时标最短,它们也是宇宙中产能最大、光变最剧烈的天体。目前标准的活动星系核统一模型认为：AGNs的中央有一个大质量黑洞,环绕该黑洞的是一个吸积盘,射电强活动星系核还会在吸积盘的旋转轴方向产生一对双向的相对论性喷流。Blazar的喷流与我们观测视线的夹角很小,喷流的辐射经过Doppler效应增强后,产生了一个下至射电波段、上至高能y-ray波段的很宽的频谱。研究Blazar天体能量的起源、传输和变化对宇宙学以及基本物理学都有重要的意义。
探索Blazar光变资料中的周期或准周期变化是一个有待深入研究的领域。由于光变资料的复杂性,目前寻找周期的算法还显得不够完善。在本论文的后半部分作者详细讨论了几种有用的周期寻找方法。
本文综述了活动星系核的基本性质和辐射机制。介绍了Blazar天体的光学观测和数据处理方法。讨论了Blazar天体的光变特性,以及光变对了解活动星系核本质的重要意义。并把经典谱估计法和现代谱估计法应用到类星体3C 279、3C 345,BL Lac天体OJ 287、ON 231的光变周期分析中,得到它们的光变周期分别为7.14年、10.00年、11.76年、6.80年。比较了各种估计方法性能之优劣,便于在实际工作中做出正确选择。获得的周期对进一步研究它们的物理机制很有帮助。
Active galactic nucleus, or AGNs, are peculiar galaxies which have energetic phenomena in the central regions. Some of the most important properties of AGNs are that they are star-like objects, have time-variable continuum spectra and broad emission lines. Variability is a common phenomenon in AGNs and is observed over wide range from radio to X-ray. It provides a powerful tool for constraining the physical mechanisms and models of the central regions of AGNs.
Blazars are radio-loud active galactic nucleus. The timescale of them is shortest in all AGNs. At the same time, they are the most powerful and the largest amplitude variable objects in the cosmos. According to the standard unified model of AGNs, there is a central massive black hole, surrounded by an accretion disk. A powerful reletivistic jet will emanate from the region near the black hole. The viewing angle of the jet of Blazar is very small. Thus, its radiation will be Doppler enhanced, and generate a wide spectrum from radio band to hight energyγ-ray band. To study Blazars energy originates, transfers and variates is very important to cosmology and basic physics.
The periodicity analysis of the light curves of Blazars needs improvement. Due to the complication of Blazars'light curves, the present periodicity analysis methods are not perfect. In the rest part of this dissertation, I disscussed in detail some suitable periodicity analysis methods.
The properties and radiation mechanisms of AGNs were reviewed. The methods of data processing and optical observation of Blazars were introduced. Then, the characteristic of Blazars variability and significance of variability for understanding the nature of AGNs were discussed. The methods that are classical spectrum estimation methods and modern spectrum estimation methods have been applied to analyze the period of the Blazar 3C 279,3C 345 and BL Lac Objects OJ 287, ON 231. Their periods are 7.14yr、10.00yr、11.76yr and 6.80yr. Moreover, their advantages and disadvantages are discussed for the practical applications. The obtained periods are helpful to understand their physical mechanisms.
Blazar天体是射电噪AGNs,在所有的AGNs中光变时标最短,它们也是宇宙中产能最大、光变最剧烈的天体。目前标准的活动星系核统一模型认为：AGNs的中央有一个大质量黑洞,环绕该黑洞的是一个吸积盘,射电强活动星系核还会在吸积盘的旋转轴方向产生一对双向的相对论性喷流。Blazar的喷流与我们观测视线的夹角很小,喷流的辐射经过Doppler效应增强后,产生了一个下至射电波段、上至高能y-ray波段的很宽的频谱。研究Blazar天体能量的起源、传输和变化对宇宙学以及基本物理学都有重要的意义。
探索Blazar光变资料中的周期或准周期变化是一个有待深入研究的领域。由于光变资料的复杂性,目前寻找周期的算法还显得不够完善。在本论文的后半部分作者详细讨论了几种有用的周期寻找方法。
本文综述了活动星系核的基本性质和辐射机制。介绍了Blazar天体的光学观测和数据处理方法。讨论了Blazar天体的光变特性,以及光变对了解活动星系核本质的重要意义。并把经典谱估计法和现代谱估计法应用到类星体3C 279、3C 345,BL Lac天体OJ 287、ON 231的光变周期分析中,得到它们的光变周期分别为7.14年、10.00年、11.76年、6.80年。比较了各种估计方法性能之优劣,便于在实际工作中做出正确选择。获得的周期对进一步研究它们的物理机制很有帮助。
Active galactic nucleus, or AGNs, are peculiar galaxies which have energetic phenomena in the central regions. Some of the most important properties of AGNs are that they are star-like objects, have time-variable continuum spectra and broad emission lines. Variability is a common phenomenon in AGNs and is observed over wide range from radio to X-ray. It provides a powerful tool for constraining the physical mechanisms and models of the central regions of AGNs.
Blazars are radio-loud active galactic nucleus. The timescale of them is shortest in all AGNs. At the same time, they are the most powerful and the largest amplitude variable objects in the cosmos. According to the standard unified model of AGNs, there is a central massive black hole, surrounded by an accretion disk. A powerful reletivistic jet will emanate from the region near the black hole. The viewing angle of the jet of Blazar is very small. Thus, its radiation will be Doppler enhanced, and generate a wide spectrum from radio band to hight energyγ-ray band. To study Blazars energy originates, transfers and variates is very important to cosmology and basic physics.
The periodicity analysis of the light curves of Blazars needs improvement. Due to the complication of Blazars'light curves, the present periodicity analysis methods are not perfect. In the rest part of this dissertation, I disscussed in detail some suitable periodicity analysis methods.
The properties and radiation mechanisms of AGNs were reviewed. The methods of data processing and optical observation of Blazars were introduced. Then, the characteristic of Blazars variability and significance of variability for understanding the nature of AGNs were discussed. The methods that are classical spectrum estimation methods and modern spectrum estimation methods have been applied to analyze the period of the Blazar 3C 279,3C 345 and BL Lac Objects OJ 287, ON 231. Their periods are 7.14yr、10.00yr、11.76yr and 6.80yr. Moreover, their advantages and disadvantages are discussed for the practical applications. The obtained periods are helpful to understand their physical mechanisms.
引文
[1]Collmar, W., et al. A large high-energy gamma-ray flare from the blazar 3C 273[J], A&A, 2000,354:513
[2]Rieger, F. M., Mannheim, K. Implications of a possible 23 day periodicity for binary black hole models in Mkn 501 [J], A&A,2000,359:948
[3]Wagner, S.J., et al. Radio Variability and Optical Variability in 0716+714[J], A&A,1992,298:688
[4]Sillanpaa, A., et al. OJ 287-Binary pair of supermassive black holes[J], ApJ,1988,325:628
[5]Sillanpaa, A., et al. Double-peak structure in the cyclic optical outbursts of blazar OJ 287[J], A&A,1996a,315:L13
[6]Sillanpaa, A., et al. Confirmation of the 12-year optical outburst cycle in blazar OJ 287[J], A&A, 1996b,305:L17
[7]Kidger, M., Takalo,l., et al. A new analysis of the 11-year period in OJ287-Confirmation of its existence[J], A&A,1992,264:32
[8]Sillanpaa, A., et al. The rise and fall of OJ 287 in 1983-1984-Periodicities and wavelength-dependent delays[J], ApSS,1991,176:297
[9]Carrasco, L., Dultzin-hacyan, D., Bruz-Gonzalez, I. Periodicity in the BL Lac object OJ287[J], Nature,1985,314:146
[10]Fan, J. H., Lin,R.G.. Optical Variability and Periodicity Analysis for Blazars.Ⅰ. Light Curves for Radio-selected BL Lacertae Objects[J], ApJ,2000,537:101
[11]Urry, C. M., Multiwavelength monitoring of the BL Lacertae object PKS 2155-304.Ⅰ-The IUE campaign[J], ApJ,1993,411:614
[12]Lainela, M., et al. The 65 Day Period in 3C 66A during Bright State[J], ApJ,1999,521:561
[13]樊军辉,2001,天文学报[J],Vol.42,No.1,9
[14]Abraham, Z., Romero, G. E., Beaming and precession in the inner jet of 3C 273[J], A&AP,1999, 344:61
[15]Fan, J. H. Infrared variability properties of the blazar 3C 279[J],1999, MNRAS,308:1032
[16]Zhang, X. et al. CCD Photometry and Long-Term Optical Variability of 3C 345[J], APSS,2000, 271
[17]Belokon, E. T., Babadzhanyants, M.K., Spectral slopes of the emission in "fast" and "slow" optical outbursts of the blazar 3C 345 [J], ApJ,1999,25:781
[18]Babadzhanyants, M. K., et al. Astronomicheskij Zhurnal, Optical monitoring of the superluminal quasar 3C 345 in 1984-1991 [J],1995,vol.72,447
[19]Chen, Y.J., Zhang, F.J., Sjouwerman, L.O. Bi-periodic variation in the BL Lac AO 0235+164[J], 1995,1999,266:495
[20]Roy,M., et al. The Recent High State of the BL Lacertae Object AO 0235 and Cross-Correlations between Optical and Radio Bands[J],2000, ApJ,545:758
[21]李启斌,李宗伟,《90年代天体物理学》[M],高等教育出版社,1996
[22]苏宜,《天文学新概论》[M],华中理工大学出版社,2000
[23]Woltijer, L. In:Courvoisier T.J.L,Mayor M.ed.Active Galactic Nuclei[M], Berlin:Spring-Verlag Press, P1
[24]周又元,袋和俊,王挺贵.90年代天体物理学[M],北京：高等教育出版社,1996,P471
[25]Peterson, B.M,《An Introduction To Active Galactic Nuclei》[M], In Cambridge University Press
[26]Woltjer, L., Emission Nuclei in Galaxies [J], APJ,1959,130:38
[27]Ghisellini, G., Extreme blazers [J], Astroparticle Physics,1999,11:11
[28]Fanaroff, B. L., Riley, J. M., Ten-micron observations of globular clusters [J], MNRAS,1974, 167:31
[29]Blandford, R. D., Rees, M. J., Extended and compact extragalactic radio sources-Interpretation and theory [J], Phys,1978,17:265
[30]Urry, C. Megan,Padovani, Paolo.Unified Schemes for Radio-Loud Active Galactic Nuclei [J], PASP,1995,107:803
[31]尤丽莎,硕士毕业论文[D],云南师范大学,2006
[32]Angel, J. R. P., Stockman, H. S.,Optical and infrared polarization of active extragalactic objects [J], ARA&A,1980,18:321
[33]Fossati, G., Ph.D., Thesis,1998,SISSA
[34]Miller, H. R.,Carini, M. T.,Goodrich, B. D., Detection of microvariability for BL Lacertae objects [J], Nature,1989,337:627
[35]Blandford, R. D., Rees, M. J., In Pittsburgh Conf. On BL Lac Objects, A.M. wolfe (Pittsburgh: Univ.Pittsburgh Press),1978,328
[36]Fugmann, W., Are all flat-spectrum radio sources Blazars [J], A&A,1988,205:86
[37]Ghisellini, G., Maraschi, L., Treves, A.,Tanzi, E. G, Spectral properties of Blazars.I-Objects observed in the far-ultraviolet.Ⅱ-an X-ray observed sample [J], ApJ,1986,310:317G
[38]Impey, C. D., Neugebauer, G, Energy distributions of Blazars [J], AJ,1988,95:3071
[39]Brown, L. M. J., Robson, E. I.,Gear, W. K., et al. Multifrequency observations of Blazars.Ⅲ-The spectral shape of the radio to X-ray continuum [J], ApJ,1989,340:129B
[40]Brown, L. M. J., Robson, E. I., Gear, W. K., Smith, M. G., Multifrequency observations of Blazars. Ⅳ-The variability of the radio to ultraviolet continuum [J], ApJ,1989,340:150B
[41]Barvainis, Richard.Hot dust and the near-infrared bump in the continuum spectra of quasars and active galactic nuclei[J], ApJ,1987,320:537B
[42]Urry, C. M., Mushotzky, R. F., Holt S S.X-ray spectroscopy of five BL Lacertae objects [J], ApJ, 1986,305:369U
[43]Giommi, P., Barr, P., Pollock, A. M. T., Garilli, B., Maccagni, D., A study of BL Lacertae-type objects with Exosat.I-Flux correlations, luminosity variability, and spectral variability[J], ApJ,1990, 356:432G
[44]Bar, P., et al.1989, in BL Lac Object[M], P290
[45]Madejskl, G M., Schwartz, D. A.,1989,in BL Lac Objects[M], P267
[46]程勇,硕士毕业论文[D],云南师范大学,2006
[47]Miller, H. R., The recent optical variability of 3C 446 [J], ApJ,1981,244:426
[48]谢光中,李开华,鲍梦贤等,6个BL Lacertae天体的短时标光变[J],1985,科学通报,23：47
[49]Bertaud, C., Wlerick, G., Veron, P., et al. Etude photometrique de BL Lacertae [J], A&A,1973, 24:357B
[50]Xie, G..Z., Zhou, S. B., Dai, B. Z.,et al. Photometric monitoring of 12 BL Lacertae objects, MNRAS,2002,329:689
[51]尤俊汉.天体物理中的辐射机制(第二版)[M],北京：科学出版社,1998,P147-263
[52]Blumenthol and Gould Bremsstrahlung. Synchrotron Radiation, and Compton Scattering of High-Energy Electrons Traversing Dilute Gases [J], Rev.Mod.Phys,1970,42:237
[53]Proakis, J. G., Manolakis, D. G., Introduction to Digital Signal Processing[M], New York: Macmillan Publishing Company,1988, P20-151
[54]A.V.Oppenheim, A.S.Willsky, and I.T.Young. Signals and Systems. Prentice-Hall[M], Englewood CliffS, NJ,1997, P35-282
[55]A. Papoulis. The Fourier Integral and its Applications[M], McGraw-Hill, New York, NY second edition,1987, P10-214
[56]吴湘淇,信号、系统与信号处理[M],北京：电子工业出版社,1996,P17-279
[57]B. Porat. Digital Processing of Random Signals:Theory and Method[M], Prentice-Hall, Englewood Cliffs, NJ,1994, P150-218
[58]M. B'Priestley. Spectral Analysis and Time Series[M], Academic Press, Boston,1981, P28-301
[59]B. Boashash, Time-frequency Signal Analysis[M], Wiley Halsted Press,1992, P120-292
[60]L. Cohen. Time-Frequency Distributions[J]:A review. Proc. IEEE, July 1989,77(7):P941-981
[61]P.Duhamel and M. Vetterli. Fast Fourier transfoms:a tutorial review and a state of the art[J], Signal Proc.,1990,19(4):P259-299,
[62]Jiang Changjin, Jiang Yong. Fast Fourier transform and C procedures. Hefei:University of Science and Technology of China Press[M],2004, P100-186
[63]Ding Yuerong, Li Zongyun. AcASn,1999,40(2):P165-172
[64]丁月蓉,郑大伟.天文测量收据的处理方法,南京：南京大学出版社[M],1990,P320-327
[65]A.V. Oppenheim, R.W.Schaffer, et al. Signal Processing[M], Prentice-Hall.Inc,1989,588
[66]Welch,P. D., The Millimeter Wave Spectrum of Saturn [J], IEEE, Trans Audio Electroacoustics, 1970,70-73
[67]Makino, F., the Ginga team. Spectral Survey of AGNs from Ginga[J], IAU circ,1988,4628
[68]Robson,E. I., Smith, et al. Blazars in 3C 279 and 3C 273 [J], IAU circ,1988,4556
[69]Kidger, M. R., Allan, P. M.,3C 279, PKS 1510-089 and OJ 287[J], IAU circ,1988,4593
[70]Makino, F., Kii, T., et al. X-ray outburst of the quasar 3C 279[J], APJ,1989,347:L9
[71]Neugebeder, G., Matthews, K., IAU circ,1988,4598
[72]Fan, J. H., Infrared variability properties of the blazar 3C 279[J], MNRAS,1999,308:1032-1036
[73]Zhang, X., Xie, G. Z., et al. CCD Photometry and Long-Term Optical Variability of 3C 345[J], APSS,2000,271
[74]Webb, J. R., et al. Optical observations of 22 violently variable extragalactic sources-1968-1986 [J], AJ,1988,95:374
[75]Schramm, K. J., Recent activity in the optical and radio lightcurves of the blazar 3C 345: indications for a'lighthouse effect'due to jet rotation[J], A&A,1993,278:391
[76]Barbieri, et al. Survey of the optical variability of compact extragalactic objects. Ⅰ-The field of 3 C 345[J], A&A,1977,59:419
[77]Zhang, X., Xie, G.Z., Bai, J. M., A historical light curve of 3C 345 and its periodic analysis[J], A&A,1998,330:469
[78]Zhang, X., Xie, G Z., Bai J M. Computing the period of light variability in BL Lac objects using the Jurkevich method[J], ChA&A,1998,18(3):P260-267
[79]Sillanpaa, A., Optical monitoring of quasars and BL Lacertae objects. Ⅱ [J], A&AS,1991, 88:225
[80]Barbieri,C., Optical variability of 16 quasi stellar objects[J], A&AS,1988,76:477
[81]曾周末,万柏坤.动态数据建模与处理[M],天津：天津大学出版社,P16-70
[82]D. J. Thomson. Spectrum estimation and harmonic analysis[J], Proc. IEEE,1982, 70:P 1055-1096.
[83]Haddad R A, Parsons T W. Digital Signal Processing:Theory, Applications, and Hardware[M], Computer Science Press,1992,P28-255
[84]Boashash, B., Estimating and interpreting the instantaneous frequency of a signal-part I: fundamentals[J], Proc. IEEE.,1992,80(4):P520-538
[85]L. Cohen., Time-frequency distributions:A review[J], Proc. IEEE, July 1989,77(7):P941-981
[86]何书元.应用时间序列分析[M],北京：北京大学出版社,P60-301
[87]L. Cohen, T. Posh. Positivity of Time-Frequency Distribution[J], IEEE Trans. On ASSP,1985, 33(1):P31-37
[88]G.W. Wornell, A.V. Oppenheim. Wavelet-based representations for a class of self similar signals with application to fractal modulation[J], IEEE Trans. Info. Theory,1992,38(2):P785-800
[2]Rieger, F. M., Mannheim, K. Implications of a possible 23 day periodicity for binary black hole models in Mkn 501 [J], A&A,2000,359:948
[3]Wagner, S.J., et al. Radio Variability and Optical Variability in 0716+714[J], A&A,1992,298:688
[4]Sillanpaa, A., et al. OJ 287-Binary pair of supermassive black holes[J], ApJ,1988,325:628
[5]Sillanpaa, A., et al. Double-peak structure in the cyclic optical outbursts of blazar OJ 287[J], A&A,1996a,315:L13
[6]Sillanpaa, A., et al. Confirmation of the 12-year optical outburst cycle in blazar OJ 287[J], A&A, 1996b,305:L17
[7]Kidger, M., Takalo,l., et al. A new analysis of the 11-year period in OJ287-Confirmation of its existence[J], A&A,1992,264:32
[8]Sillanpaa, A., et al. The rise and fall of OJ 287 in 1983-1984-Periodicities and wavelength-dependent delays[J], ApSS,1991,176:297
[9]Carrasco, L., Dultzin-hacyan, D., Bruz-Gonzalez, I. Periodicity in the BL Lac object OJ287[J], Nature,1985,314:146
[10]Fan, J. H., Lin,R.G.. Optical Variability and Periodicity Analysis for Blazars.Ⅰ. Light Curves for Radio-selected BL Lacertae Objects[J], ApJ,2000,537:101
[11]Urry, C. M., Multiwavelength monitoring of the BL Lacertae object PKS 2155-304.Ⅰ-The IUE campaign[J], ApJ,1993,411:614
[12]Lainela, M., et al. The 65 Day Period in 3C 66A during Bright State[J], ApJ,1999,521:561
[13]樊军辉,2001,天文学报[J],Vol.42,No.1,9
[14]Abraham, Z., Romero, G. E., Beaming and precession in the inner jet of 3C 273[J], A&AP,1999, 344:61
[15]Fan, J. H. Infrared variability properties of the blazar 3C 279[J],1999, MNRAS,308:1032
[16]Zhang, X. et al. CCD Photometry and Long-Term Optical Variability of 3C 345[J], APSS,2000, 271
[17]Belokon, E. T., Babadzhanyants, M.K., Spectral slopes of the emission in "fast" and "slow" optical outbursts of the blazar 3C 345 [J], ApJ,1999,25:781
[18]Babadzhanyants, M. K., et al. Astronomicheskij Zhurnal, Optical monitoring of the superluminal quasar 3C 345 in 1984-1991 [J],1995,vol.72,447
[19]Chen, Y.J., Zhang, F.J., Sjouwerman, L.O. Bi-periodic variation in the BL Lac AO 0235+164[J], 1995,1999,266:495
[20]Roy,M., et al. The Recent High State of the BL Lacertae Object AO 0235 and Cross-Correlations between Optical and Radio Bands[J],2000, ApJ,545:758
[21]李启斌,李宗伟,《90年代天体物理学》[M],高等教育出版社,1996
[22]苏宜,《天文学新概论》[M],华中理工大学出版社,2000
[23]Woltijer, L. In:Courvoisier T.J.L,Mayor M.ed.Active Galactic Nuclei[M], Berlin:Spring-Verlag Press, P1
[24]周又元,袋和俊,王挺贵.90年代天体物理学[M],北京：高等教育出版社,1996,P471
[25]Peterson, B.M,《An Introduction To Active Galactic Nuclei》[M], In Cambridge University Press
[26]Woltjer, L., Emission Nuclei in Galaxies [J], APJ,1959,130:38
[27]Ghisellini, G., Extreme blazers [J], Astroparticle Physics,1999,11:11
[28]Fanaroff, B. L., Riley, J. M., Ten-micron observations of globular clusters [J], MNRAS,1974, 167:31
[29]Blandford, R. D., Rees, M. J., Extended and compact extragalactic radio sources-Interpretation and theory [J], Phys,1978,17:265
[30]Urry, C. Megan,Padovani, Paolo.Unified Schemes for Radio-Loud Active Galactic Nuclei [J], PASP,1995,107:803
[31]尤丽莎,硕士毕业论文[D],云南师范大学,2006
[32]Angel, J. R. P., Stockman, H. S.,Optical and infrared polarization of active extragalactic objects [J], ARA&A,1980,18:321
[33]Fossati, G., Ph.D., Thesis,1998,SISSA
[34]Miller, H. R.,Carini, M. T.,Goodrich, B. D., Detection of microvariability for BL Lacertae objects [J], Nature,1989,337:627
[35]Blandford, R. D., Rees, M. J., In Pittsburgh Conf. On BL Lac Objects, A.M. wolfe (Pittsburgh: Univ.Pittsburgh Press),1978,328
[36]Fugmann, W., Are all flat-spectrum radio sources Blazars [J], A&A,1988,205:86
[37]Ghisellini, G., Maraschi, L., Treves, A.,Tanzi, E. G, Spectral properties of Blazars.I-Objects observed in the far-ultraviolet.Ⅱ-an X-ray observed sample [J], ApJ,1986,310:317G
[38]Impey, C. D., Neugebauer, G, Energy distributions of Blazars [J], AJ,1988,95:3071
[39]Brown, L. M. J., Robson, E. I.,Gear, W. K., et al. Multifrequency observations of Blazars.Ⅲ-The spectral shape of the radio to X-ray continuum [J], ApJ,1989,340:129B
[40]Brown, L. M. J., Robson, E. I., Gear, W. K., Smith, M. G., Multifrequency observations of Blazars. Ⅳ-The variability of the radio to ultraviolet continuum [J], ApJ,1989,340:150B
[41]Barvainis, Richard.Hot dust and the near-infrared bump in the continuum spectra of quasars and active galactic nuclei[J], ApJ,1987,320:537B
[42]Urry, C. M., Mushotzky, R. F., Holt S S.X-ray spectroscopy of five BL Lacertae objects [J], ApJ, 1986,305:369U
[43]Giommi, P., Barr, P., Pollock, A. M. T., Garilli, B., Maccagni, D., A study of BL Lacertae-type objects with Exosat.I-Flux correlations, luminosity variability, and spectral variability[J], ApJ,1990, 356:432G
[44]Bar, P., et al.1989, in BL Lac Object[M], P290
[45]Madejskl, G M., Schwartz, D. A.,1989,in BL Lac Objects[M], P267
[46]程勇,硕士毕业论文[D],云南师范大学,2006
[47]Miller, H. R., The recent optical variability of 3C 446 [J], ApJ,1981,244:426
[48]谢光中,李开华,鲍梦贤等,6个BL Lacertae天体的短时标光变[J],1985,科学通报,23：47
[49]Bertaud, C., Wlerick, G., Veron, P., et al. Etude photometrique de BL Lacertae [J], A&A,1973, 24:357B
[50]Xie, G..Z., Zhou, S. B., Dai, B. Z.,et al. Photometric monitoring of 12 BL Lacertae objects, MNRAS,2002,329:689
[51]尤俊汉.天体物理中的辐射机制(第二版)[M],北京：科学出版社,1998,P147-263
[52]Blumenthol and Gould Bremsstrahlung. Synchrotron Radiation, and Compton Scattering of High-Energy Electrons Traversing Dilute Gases [J], Rev.Mod.Phys,1970,42:237
[53]Proakis, J. G., Manolakis, D. G., Introduction to Digital Signal Processing[M], New York: Macmillan Publishing Company,1988, P20-151
[54]A.V.Oppenheim, A.S.Willsky, and I.T.Young. Signals and Systems. Prentice-Hall[M], Englewood CliffS, NJ,1997, P35-282
[55]A. Papoulis. The Fourier Integral and its Applications[M], McGraw-Hill, New York, NY second edition,1987, P10-214
[56]吴湘淇,信号、系统与信号处理[M],北京：电子工业出版社,1996,P17-279
[57]B. Porat. Digital Processing of Random Signals:Theory and Method[M], Prentice-Hall, Englewood Cliffs, NJ,1994, P150-218
[58]M. B'Priestley. Spectral Analysis and Time Series[M], Academic Press, Boston,1981, P28-301
[59]B. Boashash, Time-frequency Signal Analysis[M], Wiley Halsted Press,1992, P120-292
[60]L. Cohen. Time-Frequency Distributions[J]:A review. Proc. IEEE, July 1989,77(7):P941-981
[61]P.Duhamel and M. Vetterli. Fast Fourier transfoms:a tutorial review and a state of the art[J], Signal Proc.,1990,19(4):P259-299,
[62]Jiang Changjin, Jiang Yong. Fast Fourier transform and C procedures. Hefei:University of Science and Technology of China Press[M],2004, P100-186
[63]Ding Yuerong, Li Zongyun. AcASn,1999,40(2):P165-172
[64]丁月蓉,郑大伟.天文测量收据的处理方法,南京：南京大学出版社[M],1990,P320-327
[65]A.V. Oppenheim, R.W.Schaffer, et al. Signal Processing[M], Prentice-Hall.Inc,1989,588
[66]Welch,P. D., The Millimeter Wave Spectrum of Saturn [J], IEEE, Trans Audio Electroacoustics, 1970,70-73
[67]Makino, F., the Ginga team. Spectral Survey of AGNs from Ginga[J], IAU circ,1988,4628
[68]Robson,E. I., Smith, et al. Blazars in 3C 279 and 3C 273 [J], IAU circ,1988,4556
[69]Kidger, M. R., Allan, P. M.,3C 279, PKS 1510-089 and OJ 287[J], IAU circ,1988,4593
[70]Makino, F., Kii, T., et al. X-ray outburst of the quasar 3C 279[J], APJ,1989,347:L9
[71]Neugebeder, G., Matthews, K., IAU circ,1988,4598
[72]Fan, J. H., Infrared variability properties of the blazar 3C 279[J], MNRAS,1999,308:1032-1036
[73]Zhang, X., Xie, G. Z., et al. CCD Photometry and Long-Term Optical Variability of 3C 345[J], APSS,2000,271
[74]Webb, J. R., et al. Optical observations of 22 violently variable extragalactic sources-1968-1986 [J], AJ,1988,95:374
[75]Schramm, K. J., Recent activity in the optical and radio lightcurves of the blazar 3C 345: indications for a'lighthouse effect'due to jet rotation[J], A&A,1993,278:391
[76]Barbieri, et al. Survey of the optical variability of compact extragalactic objects. Ⅰ-The field of 3 C 345[J], A&A,1977,59:419
[77]Zhang, X., Xie, G.Z., Bai, J. M., A historical light curve of 3C 345 and its periodic analysis[J], A&A,1998,330:469
[78]Zhang, X., Xie, G Z., Bai J M. Computing the period of light variability in BL Lac objects using the Jurkevich method[J], ChA&A,1998,18(3):P260-267
[79]Sillanpaa, A., Optical monitoring of quasars and BL Lacertae objects. Ⅱ [J], A&AS,1991, 88:225
[80]Barbieri,C., Optical variability of 16 quasi stellar objects[J], A&AS,1988,76:477
[81]曾周末,万柏坤.动态数据建模与处理[M],天津：天津大学出版社,P16-70
[82]D. J. Thomson. Spectrum estimation and harmonic analysis[J], Proc. IEEE,1982, 70:P 1055-1096.
[83]Haddad R A, Parsons T W. Digital Signal Processing:Theory, Applications, and Hardware[M], Computer Science Press,1992,P28-255
[84]Boashash, B., Estimating and interpreting the instantaneous frequency of a signal-part I: fundamentals[J], Proc. IEEE.,1992,80(4):P520-538
[85]L. Cohen., Time-frequency distributions:A review[J], Proc. IEEE, July 1989,77(7):P941-981
[86]何书元.应用时间序列分析[M],北京：北京大学出版社,P60-301
[87]L. Cohen, T. Posh. Positivity of Time-Frequency Distribution[J], IEEE Trans. On ASSP,1985, 33(1):P31-37
[88]G.W. Wornell, A.V. Oppenheim. Wavelet-based representations for a class of self similar signals with application to fractal modulation[J], IEEE Trans. Info. Theory,1992,38(2):P785-800