New Insights into Betelgeuse's Inhomogeneous Wind

Details New Insights into Betelgeuse's Inhomogeneous Wind New Insights into Betelgeuse's Inhomogeneous Wind

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003hst..prop.9928h&link_type=abstract

HST Proposal ID #9928

Physics

Hst Proposal Id #9928 Cool Stars

Scientific paper

Our understanding of the physical causes of mass loss from evolved late-type stars has been stymied by the lack of observations that resolve the wind acceleration region. Recently both multi-wavelength cm-radio and STIS UV observations of Alpha Orionis {M2 Iab} have been obtained that probe these crucial spatial scales. Our recent 2002 cm-radio VLA + Pie Town data show that the vast majority of the inner wind is much cooler {1500 K} than the 5000-8000 K predicted from previous UV observations. A volume of hot plasma must, however, be present to explain the UV emission. An understanding of such inhomogeneous winds is a prerequisite to advances in determining the nature of the mass loss process in M supergiants. Using VLA data we made the first step towards a mean description of the complex atmosphere {Harper, Brown & Lim 2001 ApJ 551, 1073}, and now we propose to use STIS E230M spatial scans of Alpha Ori to construct the first detailed thermodynamic multi-component model. The 25x100 mas aperture scans provide the first opportunity to truly resolve the wind acceleration region and probe the enigmatic hot plasma which is the site additional heating. Using state-of-the-art analysis tools, we will empirically determine, for the first time, the electron and hydrogen density as a function of position {and velocity} and empirically determine the geometry and filling factor of the hot plasma. This detailed model will allow us test the proposed mechanisms for mass loss and heating.

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