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MULTIWAVELENGTH VARIABILITY PROPERTIES OF FERMI BLAZAR S5 0716+714
Liao NH(廖能惠)1,2,3; Bai JM(白金明)1,2; Liu HT(刘洪涛)1,2; Weng, SS4; Chen, L5; Li F(李璠)1,2; Liao, NH (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Yunnan, Peoples R China.
发表期刊ASTROPHYSICAL JOURNAL
2014-03-10
卷号783期号:2页码:83-99
DOI10.1088/0004-637X/783/2/83
产权排序第1完成单位
收录类别SCI
关键词Bl Lacertae Objects: Individual Galaxies: Active Galaxies: Jets Radiation Mechanisms: Non-thermal
摘要S5 0716+714 is a typical BL Lacertae object. In this paper we present the analysis and results of long-term simultaneous observations in the radio, near-infrared, optical, X-ray, and gamma-ray bands, together with our own photometric observations for this source. The light curves show that the variability amplitudes in gamma-ray and optical bands are larger than those in the hard X-ray and radio bands and that the spectral energy distribution (SED) peaks move to shorter wavelengths when the source becomes brighter, which is similar to other blazars, i. e., more variable at wavelengths shorter than the SED peak frequencies. Analysis shows that the characteristic variability timescales in the 14.5 GHz, the optical, the X-ray, and the gamma-ray bands are comparable to each other. The variations of the hard X-ray and 14.5 GHz emissions are correlated with zero lag, and so are the V band and gamma-ray variations, which are consistent with the leptonic models. Coincidences of gamma-ray and optical flares with a dramatic change of the optical polarization are detected. Hadronic models do not have the same natural explanation for these observations as the leptonic models. A strong optical flare correlating a. -ray flare whose peak flux is lower than the average flux is detected. The leptonic model can explain this variability phenomenon through simultaneous SED modeling. Different leptonic models are distinguished by average SED modeling. The synchrotron plus synchrotron selfCompton (SSC) model is ruled out because of the extreme input parameters. Scattering of external seed photons, such as the hot-dust or broad-line region emission, and the SSC process are probably both needed to explain the gamma-ray emission of S5 0716+714.
项目资助者Fermi Guest Investigato [NNX08AW56G, NNX09AU10G, NNX12AO93G] ; University of Michigan ; 973 Proagram [2009CB824800] ; National Natural Science Foundation of China (NSFC) [11133006, 11273052, 11233006, 11173043, 11133002, 11303022, 11103060] ; Youth Innovation Promotion Association, CAS ; National Science Foundation [AST-0607523]
语种英语
学科领域Astronomy & Astrophysics
文章类型Article
ISSN0004-637X
URL查看原文
归档日期2014-05-06
WOS记录号WOS:000335439900019
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]ACTIVE GALACTIC NUCLEI ; LARGE-AREA TELESCOPE ; BL-LACERTAE OBJECTS ; TERM OPTICAL VARIABILITY ; RAPID TEV VARIABILITY ; RAY BRIGHT BLAZARS ; LAC OBJECTS ; INTRADAY VARIABILITY ; GAMMA-RAYS ; PHYSICAL-PROPERTIES
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被引频次:30[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/5446
专题丽江天文观测站(南方基地)
中国科学院天体结构与演化重点实验室
通讯作者Liao, NH (reprint author), Chinese Acad Sci, Yunnan Observ, Kunming 650011, Yunnan, Peoples R China.
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, Kunming, Yunnan 650011, China
2.Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, Yunnan 650011, China
3.University of Chinese Academy of Sciences, Beijing 100049, China
4.Department of Physics, Xiangtan University, Xiangtan 411105, China
5.Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China
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Liao NH,Bai JM,Liu HT,et al. MULTIWAVELENGTH VARIABILITY PROPERTIES OF FERMI BLAZAR S5 0716+714[J]. ASTROPHYSICAL JOURNAL,2014,783(2):83-99.
APA Liao NH.,Bai JM.,Liu HT.,Weng, SS.,Chen, L.,...&Liao, NH .(2014).MULTIWAVELENGTH VARIABILITY PROPERTIES OF FERMI BLAZAR S5 0716+714.ASTROPHYSICAL JOURNAL,783(2),83-99.
MLA Liao NH,et al."MULTIWAVELENGTH VARIABILITY PROPERTIES OF FERMI BLAZAR S5 0716+714".ASTROPHYSICAL JOURNAL 783.2(2014):83-99.
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