Physics
Scientific paper
Feb 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..888r&link_type=abstract
COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.
Physics
Giant And Subgiant Stars, Stellar Activity, Stellar Characteristics And Properties
Scientific paper
As a star cools and expands to become a red giant it will become pulsationally unstable. The amplitude tends to increase with decreasing temperature as the star ascends the red giant branch. Below around 4,000 K (Spectral Type K5III) microvariability sets in. This may have a strong impact on the pulsation-driven mass loss history. We are studying a sample of symbiotic binaries in order to understand the mechanism of mass loss from the red giant primary. Photometric monitoring indicates small-scale variability of around 20% over a timescale of ~30 days. This is likely related to the convective motion on the surface which may be directly or indirectly involved in providing the initial impetus to raise material and initiate the wind. Studying this convective motion and its relationship with the wind will improve our understanding of the wind's origin.
Crowley Cian
Espey Brian R.
Roche Joseph
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