Winds in R Coronae Borealis Stars

Details Winds in R Coronae Borealis Stars Winds in R Coronae Borealis Stars

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..313..569c&link_type=abstract

Asymmetrical Planetary Nebulae III: Winds, Structure and the Thunderbird, Proceedings of the conference held 28 July - 1 August

Astronomy and Astrophysics

Astronomy

Scientific paper

We present new spectroscopic observations of the He I λ10830 line in R Coronae Borealis (RCB) stars which
provide the first strong
evidence that most, if not all, RCB stars have winds. It has long been suggested that when dust forms around an RCB star, radiation pressure accelerates the dust away from the star, dragging the gas along with it. The new spectra show that all of the ten stars observed have P-Cygni or asymmetric blue-shifted profiles in the He I λ10830 line. In all cases, the He I line indicates a mass outflow - with a range of intensity and velocity. Around the RCB stars, it is likely that this state is populated by collisional excitation rather than photoionization/recombination.

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