Radio Emissions from Companions to Cool Giant Stars

Details Radio Emissions from Companions to Cool Giant Stars Radio Emissions from Companions to Cool Giant Stars

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21537704i&link_type=abstract

American Astronomical Society, AAS Meeting #215, #377.04; Bulletin of the American Astronomical Society, Vol. 42, p.586

Astronomy and Astrophysics

Astronomy

Scientific paper

A number of substellar companions to evolved cool stars have now been reported. Cool giants differ from their progenitor Main Sequence stars in significant ways: their mass-loss rates are orders of magnitude larger and KM giant star winds are largely neutral. The latter means that the late type stellar winds penetrate the magnetospheres of low mass companions to form a bow shock morphology at the companion. We report on the radio emissions from substellar companions to giant stars using (a) the radiometric Bode's law for earlier coronal-type giant star winds and (b) a model for a bow shock morphology for latter non-coronal type giant star winds. We suggest that for high mass-loss stars, such as AGB stars, the decametric radio emissions may be a new way to identify planetary systems at late stages of stellar evolution.
This research was funded in part by a grant from the National Science Foundation, AST-0936427.

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