| OJ 287,0716+714与BL Lacertae的光变分析 |
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| 引用本文： | 王洪涛,潘艳平.OJ 287,0716+714与BL Lacertae的光变分析[J].天文学报,2012,53(4):265-273. |
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| 作者姓名： | 王洪涛 潘艳平 |
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| 作者单位： | 1. 廊坊师范学院物理与电子信息学院 廊坊065000
2. 中国科学院云南天文台 昆明650011;福建工程学院数理系 福州350108 |
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| 基金项目： | 廊坊师范学院科学研究项目，廊坊市科学技术研究与发展计划项目 |
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| 摘 要： | OJ 287是存在着剧烈活动的低峰频BL Lac天体,其低频段的能谱与另两个TeV BL Lac天体(0716+714和BL Lacertae)在低频段的能谱很相似,但是切仑科夫望远镜却没能探测到它的TeV射线.利用这3个天体的观测数据,比较它们在22 GHz、37 GHz和B波段的最小光变周期及延迟的异同,进一步寻找没有观测到OJ 287的TeV伽马射线的可能原因.分析结果显示:(1)最小光变周期方面,OJ 287在37 GHz和B波段的周期偏小,在22 GHz,OJ 287与0716+714的结果相当,但与BL Lacertae相比要小很多,OJ 287的周期更短表明其活动性更强,却没有探测到来自OJ 287的TeV伽马射线,这表明OJ 287在TeV波段的辐射与这3个低能波段最小光变周期之间可能没有联系;(2)延迟方面,OJ 287在B波段相对于37 GHz的延迟要长于0716+714,短于BL Lacertae;在37 GHz相对于22 GHz的延迟要短于0716+714,而BL Lacertae在37 GHz相对于22 GHz的时延为负值,表明22 GHz要超前于37 GHz.通过对延迟的比较分析,并没有发现OJ 287与0716+714和BL Lacertae之间存在明显的差异;从能谱来看,很可能是由于OJ 287在TeV波段的能谱较陡造成切仑科夫望远镜没有探测到来自OJ 287的伽马辐射,但TeV能段较陡的能谱对低能段光变的影响目前还不是很清楚.
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| 关 键 词： | 类星体:个别 星系:基本参数 方法:分析 |
Comparison and Analysis of Light Variations of OJ 287,0716+714 and BL Lacertae |
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| WANG Hong-tao
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PAN Yan-ping.Comparison and Analysis of Light Variations of OJ 287,0716+714 and BL Lacertae[J].Acta Astronomica Sinica,2012,53(4):265-273. |
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| Authors: | WANG Hong-tao PAN Yan-ping |
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| Institution: | (2,3) (1 Physics and Electronics Information College,Langfang Teachers’ College,Langfang 065000) (2 Yunnan Astronomical Observatory,Chinese Academy of Sciences,Kunming 650011) (3 Department of Mathematics and Physics,Fujian University of Technology,Fuzhou 350108) |
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| Abstract: | Abstract OJ 287 is a low peak frequency BL Lac object with violent actions.Its energy spectrum distribution(SED) in low frequency is similar to the other two TeV BL Lac objects(0716+714 and BL Lactertae).However,its TeV gamma rays are not detected by the Cherenkov telescopes.We compare the differences and similarities in the aspects of the minimum variation period and time delay among 22 GHz,37 GHz and B band.The causes of OJ 287 without detected TeV gamma rays are studied and analyzed.The results are as follows:(1) In 37 GHz and B band,the minimum variability periods of OJ 287 are smaller than those of the other two objects,respectively.In 22 GHz,the minimum variability period of OJ 287 is comparable to 0716+714,but is much smaller than that of BL Lacertae.Though with smaller variation period,we can not detect the TeV gamma rays from OJ 287.It is shown that the radiation from OJ 287 in TeV band is possibly not related to the minimum variation period in 22 GHz,37 GHz and B band.(2) The time delay of OJ 287 in B band relative to 37 GHz is longer than that of 0716+714,but shorter than that of BL Lacertae.The time delay of OJ 287 at 37 GHz relative to 22 GHz is shorter than that of 0716+714.The corresponding time delay of BL Lacertae is negative,which means that the radiation at 22 GHz leads the radiation at 37 GHz.By comparing and analyzing the results in time delay,we can not find some obvious differences among OJ 287, 0716+714 and BL Lacertae.It is probable that the SED of OJ 287 is steeper than others, which leads to the undetected TeV gamma ray radiation with the Cherenkov telescopes.It is still unknown how the SED in TeV band affects the light variation in the low energy band. |
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| Keywords: | quasars individual galaxies fundamental parameters methods analytical |
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