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BL Lac 天体OJ 287 是一个重要的Blazar天体, 光变具有准周期特点. 本文从密歇根大学射电天文台数据库收集了OJ 287射电波段4.8, 8.0和 14.5 GHz超过30年时间的观测数据. 由于天文观测资料的复杂性, 一些传统寻找周期的方法不是太理想. 近几年迅速发展起来的聚合经验模态分解(EEMD) 特别适合于具有非线性和非平稳动态变化特性的Blazar天体光变规律的研究. 运用EEMD方法对OJ 287 的3个射电波段流量分别进行多时间尺度分解, 各获得6个代表不同时间尺度局部特征信息的本征模态函数分量和一个趋势项. 研究结果表明: 4.8 GHz射电流量变化的主要周期是18.9, 11.9, 5.7 和2.4年; 8.0 GHz 的主要周期是12.2, 5.2和2.4 年; 14.5 GHz的主要周期是21.8, 12.0, 4.3和 2.4 年. 尽管3个波段流量变化主要周期大小有一定的差别, 但是存在着近似相同的变化周期12.0 和2.4年, 说明这3个波段可能来源于相同的辐射机制, 也证实了OJ 287 射电波段和光学波段具有相同的长光变周期12.0 年. 这些结论表明: EEMD 作为一种全新的非线性、非平稳信号处理方法, 可以更精确地提取Blazar天体中不同光变周期的分量.BL Lacertae object OJ 287 is one of the Blazars, which shows convincing evidence of periodic variations. We have collected the 4.8, 8.0 and 14.5 GHz data for OJ 287 from the University of Michigan Radio Observatory database over three decades. Due to the complexity of the variability data, some algorithms for period searching are not ideal yet. An alternative to traditional periodicity analysis is the ensemble empirical mode decomposition (EEMD). This method can analyze the cyclic components of complicated nonlinear and non-stationary processes. Using the EEMD analysis, the light curve of OJ 287 at radio frequency can be resolved into six independent intrinsic mode functions that have different average periods and trends. We find possible periods of 18.9, 11.9, 5.7 and 2.4 years in 4.8 GHz, 12.2 , 5.2 and 2.4 years in 8.0 GHz and 21.8, 12.0, 4.3 and 2.4 years in 14.5 GHz. The most common periods are 12.0 years and 2.4 years, which imply that the emissions in these bands may originate from the same radiative process. The results also confirm that a radio variability period of OJ 287 is in agreement with the optical variability period of about 12.0 years. The result shows that the components of different variability periods can be separated properly with the EEMD that is a nonlinear and non-stationary signal processing method.
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Keywords:
- OJ 287 /
- variability period /
- ensemble empirical mode decomposition
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[1] Tang J, Wu X B 2011 Acta Phys. Sin. 60 119801 (in Chinese) [唐洁, 吴学兵 2011 60 119801]
[2] Tang J, Fu M X, Wu X B 2012 Acta Phys. Sin. 61 219501 (in Chinese) [唐洁, 傅明星, 吴学兵 2012 61 219501]
[3] Valtonen M J, Lehto H J, Nilsson K, Heidt J Takalo L O 2008 Nature 452 850
[4] Fan J H, Zhang Y W, Qian B C, Tao J, Liu Y, Hua T X 2009 Astrophys. J. Suppl. Ser.181 466
[5] Zhang H J, Zhao G, Zhang X, Bai J M 2010 Sci. China G 53 252
[6] Huang N E, Shen Z, Long S R 1998 Proc. Royal Soc. London A 454 903
[7] Zhao H W, Huang N E 2004 Proc. Royal Soc. London A 460 1597
[8] Fan J H, Liu Y, Qian B C, Tao J, Shen Z Q, Zhang J S, Huang Y, Wang J 2010 Res. Astron. Astrophys. 10 1100
[9] Dai B Z, Li X H, Liu Z M, Zhang B K, Na W W, Wu Y F, Hao J M 2009 Mon. Not. R. Astron. Soc. 392 1181
[10] Dai B Z, Zhang B K, Zhang L 2006 New Astron. 11 471
[11] Tang J, Zhang X 2010 Acta Phys. Sin. 59 7516 (in Chinese) [唐洁, 张雄2010 59 7516]
[12] 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
[13] Tang J 2012 Acta Astron. Sin. 53 1 (in Chinese) [唐洁 2012 天文学报 53 1]
[14] Sillanpää A, Haarala S, Valtonen M J, Sundelius B, Byrd G G 1988 Astrophys. J. 325 628
[15] Sillanpää A, Takalo L O, Pursimo T, Nilsson K, Heinamaki P, Katajainen S 1996 Astron. Astrophys. 305L 13
[16] Valtonen M, Kidger M, Lehto H, Poyner G 2008 Astron. Astrophys. 477 407
[17] Xie G Z, Yi T F, Li H Z, Zhou S B, Chen L E 2008 Astron. J. 135 2212
[18] Zhang X, Zheng Y G, Zhang H J, Liu Y, Wen Y B, Wang W 2008 Astron. J. 136 1846
[19] Venturi T, Dallacasa D, Orfei A 2001 Astron. Astrophys. 379 755
[20] Boettcher M Fultz K, Aller H D 2009 Astrophys. J. 694 174
[21] Raiteri C M Villata M, Larionov V M 2008 Astron. Astrophys. 480 339
[22] Bai J M, Lee M G 2003 Astrophys. J. 585L 113
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