Links Between Hot Stars and Their Disks

Details Links Between Hot Stars and Their Disks Links Between Hot Stars and Their Disks

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..178r&link_type=abstract

The Nature and Evolution of Disks Around Hot Stars, ASP Conference Series, Vol. 337, Proceedings of a meeting held 7-9 July 2004

Physics

4

Scientific paper

The lifecycles of classical Be star disks are reviewed from an observer's point of view, presenting the spectroscopic evidence concerning the disk formation, evolution, and dissipation. With the exception of hydrodynamic processes during the gradual evolution, all these phases are driven or influenced rather directly by stellar processes. For the disk formation, the stellar processes concerned are rotation, pulsation, and possibly magnetic fields. In particular, the question what fraction is contributed by rotation has been re-opened recently. The disk formation proper, the outburst, has been observed as being rather a discrete than steady process. During the outburst the direct physical connection between star and disk also influences the stellar variability itself. Once the outburst ends, the disk enters a phase of gradual outward evolution. With time, the inner regions of the disk become thinner, turning the disk into a ring with an increasing inner radius. If not replenished by subsequent outbursts, the disk will finally dissipate into the interstellar gas.

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