Structure and Evolution of Quasi-Stellar Radio Sources
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概要
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The recently improved observational data on the quasi-stellar radio sources (QSS) and on the radio galaxies are analyzed to put forward the theory of the structure and evolution of QSS, along the model proposed by Aizu, Fujimoto, Hasegawa, Kawabata and Taketani (AFHKT). It results from the present analysis that the model proposed by AFHKT is confirmed generally by the recent data. In the course of the present analysis, we are led to propose the non-uniform model of the nucleus of galaxy, in which local condensations with stars and gas are assumed to exist. Explosions taking place successively and/or simultaneously in the condensations, are shown to account for the essential features of the QSS. Constructing renewedly the luminosity L versus volume emissivity L/V diagram from the recent data, it is found that there exists an upper envelope under which almost all the plotted sources are located. The evolutional path along the upper envelope is seen to be divided into three stages, that is, the optical, radio and remnant stages. The optical stage corresponds to the formation of the core with size of ~1 Kpc. During this stage many small components with size of ~1 pc, which are formed by the explosion of condensations, appear successively. The radio stage corresponds to the formation of the halo, and finally the remnant stage to the expansion of the halo with size of ~50 Kpc. A characteristic feature newly found here about the evolutional path along the upper envelope is that the luminosity is nearly constant during the optical and radio stages. The upper envelope has a slope of about 1/2 during the remnant stage as was discussed by Aizu, Fujimoto, Hasegawa and Taketani. In order to explain the flat part of the evolution of QSS along the upper envelope a non-uniform structure of the radio core is proposed which is composed of clouds or filaments. From a statistical analysis it is concluded that the evolution of QSS along the upper envelope is a special case and most of QSS leave the upper envelope during the radio stage with the decreasing luminosity. It is found that there are two groups of QSS which are named as the Q and G group. It is swoun that the optical phenomena associated with QSS in the G group can be considered to be independent of its present radio emission and to be due to a new explosion. It is pointed out that the optical properties of QSS in the G group may be similar to those of QSS in the Q group or to those of the quasi-stellar galaxies (QSG).
- 理論物理学刊行会の論文
- 1968-12-25
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関連論文
- L-(L/V) Diagram of Supernovae and Some Related Problems
- Structure and Evolution of Quasi-Stellar Radio Sources