Relay-Version: version B 2.10 5/3/83; site utzoo.UUCP Posting-Version: version B 2.10.1 6/24/83; site astrovax.UUCP Path: utzoo!linus!philabs!cmcl2!floyd!vax135!houxz!houxm!ihnp4!astrovax!elt From: elt@astrovax.UUCP (Ed Turner) Newsgroups: net.physics,net.astro.expert Subject: Re: pulsing quasars and the like Message-ID: <366@astrovax.UUCP> Date: Mon, 4-Jun-84 10:27:41 EDT Article-I.D.: astrovax.366 Posted: Mon Jun 4 10:27:41 1984 Date-Received: Wed, 6-Jun-84 00:59:06 EDT References: <2631@ecsvax.UUCP> Organization: Princeton Univ. Astrophysics Lines: 14 In the example of a source consisting of a central exciter and a peripheral emitter, the duration of the observed pulse will still be of order the light travel time size of the object because of the delays in propogating any signal (pulse) across the emitter. In other words, the observer will see the near side of the source light up at a time D/c (where D is the emitter's diameter) before the light from the far side of the source arrives. By properly phasing the emission from different regions on the emitting surface, observers in some particular direction can see a pulse much narrower than D/c but this will cause other observers to see even longer pulses so the mean will still be of order D/c. Ed Turner astrovax!elt