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Spiral shocks in astrophysical disks

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Original languageEnglish
Title of host publicationTHE PHYSICS OF COLLISIONLESS SHOCKS
Subtitle of host publication4th Annual IGPP International Astrophysics Conference
PublisherAIP PRESS
Pages325-330
Volume781
Publication statusPublished - 1 Aug 2005

Abstract

Spiral shocks waves are present in many astrophysical systems, including galactic disks, binary systems such as cataclysmic variables, AGN disks, and are probably present in disks around newly forming stars. In this paper we will discuss, in particular, spiral shocks resulting from the growth of a gravitational instability. We investigate how these spiral waves can transport angular momentum outwards and mass inwards - an important aspect of star formation - and a process that may play a role in the secular evolution of disk galaxies, leading to the formation of bulges. In some cases the instability can be sufficiently violent for the disk to fragment into gravitationally bound objects. This may explain the origin of the stellar population orbiting the galactic center, and has also been suggested as a mechanism for forming gaseous planets similar to Jupiter and Saturn. We consider the conditions required for fragmentation and whether such a process could indeed produce gaseous planets.

    Research areas

  • shock waves, accretion disks, star formation, galaxies, cataclysmic binary stars, galactic nuclei, Star formation, Accretion and accretion disks, Infall accretion and accretion disks, Cataclysmic binaries, symbiotic stars

ID: 19690430