Understanding the Thermodynamics of late-K and early-M Supergiant Winds

Details Understanding the Thermodynamics of late-K and early-M Supergiant Winds Understanding the Thermodynamics of late-K and early-M Supergiant Winds

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005sptz.prop20045h&link_type=abstract

Spitzer Proposal ID #20045

Physics

Scientific paper

Mass loss from evolved cool stars is an important ingredient for both galactic chemical and stellar evolution, yet the mechanisms which drive mass loss remain a mystery. Most of the energy and momentum is deposited into the wind close to the star where the acceleration takes place. We propose to obtain Long- and Short High R~600, 10-37 micron spectra of a sample of late-K and early-M supergiants which probe this key spatial region, where the mass loss mechanisms will be most manifest. Emission line diagnostics will provide thermodynamic constraints on the envelopes, and provide important insights into the unknown mechanisms which heat and drive the stellar winds. These spectra will also reveal how the envelope properties change with spectral-type at the onset of dust formation in these supergiant winds.

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