Radiative Collimation of Electron-Positron Jets

Details Radiative Collimation of Electron-Positron Jets Radiative Collimation of Electron-Positron Jets

Jun 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001pasj...53..555f&link_type=abstract

Publications of the Astronomical Society of Japan, vol.53, no. 3, p. 555-563

Astronomy and Astrophysics

Astronomy

17

Accretion, Accretion Disks, Accretion-Disk Winds, Astrophysical Jets, Electron-Positron Pair Plasmas, X-Rays: Individual (Ss 433, 1E 1740.7-2942, Grs 1915+105, Gro J1655-40)

Scientific paper

We propose a novel mechanism for the collimation of relativistic outflows emanated from accretion disks via the disk radiation field, itself. In general, winds driven by disk radiation fields diverge, due to the effect of rotation and the nature of radiation. If, however, the disk is divided into an optically thin hot inner region and an optically thick luminous outer region, the outflow ejected from the inner disk is accelerated and collimated by radiation fields produced by the outer disk. Since this mechanism effectively works on electron-positron pair plasmas, in accretion disk systems with inner hot advection-dominated regions, electron-positron jets easily form on the disk-rotation axis. For pure electron-positron pair plasmas, the terminal speed of collimated jets is about 0.9c, which is very close to the jet speed of galactic superluminal sources.

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