Structure and evolution of pulsating hot subdwarfs

Abstract

Hot subdwarfs are evolved low--mass stars that have survived core helium ignition and are now in (or recently finished with) the core helium burning stage. At the hot end of the Horizontal Branch (HB), many of these stars are multiperiodic pulsators. These pulsations have revealed details of their global and internal structure, and provide important constraints on the origin of hot HB stars. While many features of their structure deduced from seismic fits have confirmed what we expected from evolutionary considerations, there have been some surprises as well.

6 pages, invited review from Fourth HELAS International Conference: Seismological Challenges for Stellar Structure (February 2010)

References in corpus (3)

• Abundance studies of sdB stars using UV echelle HST/STIS spectroscopy
• Mass-loss and diffusion in subdwarf B stars and hot white dwarfs: do weak winds exist?
• A seismic approach to testing different formation channels of subdwarf B stars

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• Orbital Characteristics of the Subdwarf-B and F V Star Binary EC~20117-4014(=V4640 Sgr)