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Periodicity and Luminosity of the ‘Pulsar’ Model of Quasars

Published online by Cambridge University Press:  07 February 2017

William A. Fowler
William A. Fowler*
Affiliation:
Institute of Theoretical Astronomy Cambridge, U.K. California Institute of Technology Pasadena, Calif., U.S.A.

Abstract

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The diagnosis of pulsar-like symptoms in the quasar 3C 345 has renewed interest in differentially rotating supermassive stars (SMS). Quasi-periodic behavior follows from differential rotation. In reviewing early work on this quasar model it is found that SMS models with rotational periods of the order of a few hundred days and with pulsation periods approximately one-quarter as long can supply thermal and magnetic dipole radiation of the order of 1048 erg sec-1 for somewhat more than 106 yr. The surface field required for the magnetic dipole radiation is approximately 103 G. The SMS mass taken as typical in the calculations is 3 × 109M⊙.

Type
Session 6
Information
Symposium - International Astronomical Union , Volume 46: The Crab Nebula , 1971 , pp. 364 - 377
Copyright
Copyright © Reidel 1971 

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