Hostname: page-component-cd9895bd7-p9bg8 Total loading time: 0 Render date: 2024-12-25T15:47:32.203Z Has data issue: false hasContentIssue false
  • English
  • Français

The Relativistic Beaming Model and Superluminal Motions1

Published online by Cambridge University Press:  12 April 2016

J. H. Fan ,
G.Z. Xie ,
Y.H. Zhang  and
Y.P. Qin
J. H. Fan
Affiliation:
Center for Astrophysics, Guangzhou Normal University, Guangzhou 510400, China
G.Z. Xie
Affiliation:
Yunnan Observatory, The Chinese Academy of Science, Kunming, China
Y.H. Zhang
Affiliation:
Yunnan Observatory, The Chinese Academy of Science, Kunming, China
Y.P. Qin
Affiliation:
Yunnan Observatory, The Chinese Academy of Science, Kunming, China

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

In this paper, we consider a compilation of 55 objects with known superluminal motions (SM), and whose flux density (X-ray, optical, radio), core dominance parameter (R), superluminal velocity, and radio Doppler factor (δR) are known. Our study shows that SM is consistent with the beaming model, and the relation

is reasonable. The statistical correlation between superluminal velocity and redshift is a result of selection and the statistical correlation between R and brightness temperature (Tob) is actually a reflection of the correlations between δ, R, and Tob for objects with SM. Up to now, 59 objects have been reported to have SM, but for reasons discussed elsewhere (Vermeulen & Cohen 1994), only 55 are considered here.

Type
I. X-Rays and the Nuclear Regions of Active Galaxies
Information
International Astronomical Union Colloquium , Volume 159: Emission Lines in Active Galaxies: New Methods and Techniques , 1997 , pp. 74 - 75
Copyright
Copyright © Astronomical Society of the Pacific 1997

Footnotes

1

This work is supported by the National Natural Science Foundation of China and the Natural Science Foundation of Guangdong Province.

References

Fan, J.H., et al. 1993, ApJ, 415, 113.Google Scholar
Fan, J.H., et al. 1994, ApSS, 213, 305.Google Scholar
Fan, J.H., et al. 1996, A&AS, 116, in press.Google Scholar
Fan, J.H., & Xie, G.Z. 1996, A&A, 306, 55.Google Scholar
Padovani, P. 1992, A&A, 256, 399.Google Scholar
Vermeulen, R.C., & Cohen, M.H. 1994, ApJ, 430, 467.Google Scholar
Xie, G.Z., et al. 1995, ApJ, 454, 50.CrossRefGoogle Scholar