摘要： The Cerenkov line-like radiation in a dense gas (N sub(H) > 10 super(13) cm sub(-3)) is potentially important in the exploration of the optical broad emission lines of quasars and Seyfert 1 galaxies.With this quasi-line emission mechanism, some long standing puzzles in the study of quasars could be resolved. In this paper, we calculate the power of the Cerenkov line-like radiation in dense gas and compare with the powers of other radiation mechanisms by a fast electron to confirm its importance. From the observed gamma-ray luminosity of 3C 279, we show that the total number of fast electrons is sufficiently high to allow effective operation of the quasi-line emission.We present a model calculation for the luminosity of the Cerenkov Ly alpha line of 3C 279, which is high enough to compare with observations. We therefore conclude that the broad line of quasars may be a blend of the Cerenkov emission line with the real line produced by the bound-bound transition. A new approach to the absorption of the Cerenkov line is presented with the method of escape probability, which markedly simplifies the computation in the optically thick case. The revised set of formulae for the Cerenkov line-like radiation is more convenient in applications. 出版者： United States 出版日期： 2014-01-01 出處： The Astrophysical journal, 2014-01, Vol.780 (1), p.89-12 資源來源： Institute of Physics Journals 識別號： ISSN: 0004-637X 識別號： ISSN: 1538-4357 識別號： EISSN: 1538-4357 識別號： DOI: 10.1088/0004-637X/780/1/89
