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Variability investigation of quasars 4C 38.41 and 3C 345 at 92 cm: additional 14 observations
Peng, B
2002-02-21
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume330Issue:2Pages:344-348
AbstractThis paper provides additional evidence for the variability of the quasar 4C 38.41 based on 14 short observations at 92 cm using the Westerbork Synthesis Radio Telescope (WSRT). A fractional variability of 11.6 per cent was observed during the periods of 1989 May and from 1992 December to 1993 May. A brightness temperature or T-B similar to 2.6 or 5.2 x 10(18) delta(-3) K in 4C 38.41 can be estimated in the comoving frame, far in excess of the inverse Compton limit 10(12) K. A Doppler factor of delta greater than or equal to 138 would be required by invoking the relativistic bulk motion. Combining the published six Westerbork North Sky Survey (WENSS) mosaic data at 92 cm, we conclude that 4C 38.41 has significant variability, which is unlikely to be caused by propagation effects. No variability was found for the quasar 3C 345.
KeywordRadiation Mechanisms : Non-thermal Scattering Methods : Data Analysis Quasars : Individual : 4c 38.41 Quasars : Individual : 3c 345 Radio Continuum : Galaxies
Indexed BySCI
Language英语
WOS IDWOS:000174155100012
Citation statistics
Cited Times:2[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/8543
Collection射电天文研究部
AffiliationChinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China
Recommended Citation
GB/T 7714
Peng, B. Variability investigation of quasars 4C 38.41 and 3C 345 at 92 cm: additional 14 observations[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2002,330(2):344-348.
APA Peng, B.(2002).Variability investigation of quasars 4C 38.41 and 3C 345 at 92 cm: additional 14 observations.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,330(2),344-348.
MLA Peng, B."Variability investigation of quasars 4C 38.41 and 3C 345 at 92 cm: additional 14 observations".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 330.2(2002):344-348.
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