The following document lists the file abstract/PHAUSCHI_PH_SL_FA.abs
from catalogue VI/111.
A plain copy of the file
(without headers/trailers) may be downloaded.
We propose to obtain SWS spectra around the 3micron wavelength region with R 1700 for a sample of red dwarf stars. The spectra will show strong features primarily due to photospheric water absorption; the stars have a range of effective temperature and metallicity and we will measure the dependence of the absorption features on these parameters. We will analyse the data using our new state-of-the-art model atmospheres for M dwarfs, which include a detailed line-by-line treatment of water. ISO observations of the water bands are crucial for increasing our knowledge of these cool, high-pressure, stellar atmospheres. Water vapour is thought to be the dominant opacity source in very low mass dwarf stars but it is extremely difficult to quantify from the Earth due to the presence of the terrestrial water bands. ISO will allow us for the first time to determine the depth of the stellar water bands. Analysing the ISO spectrum using our new models will lead to vast improvements in our understanding of opacity sources, chemical composition, effective temperature, pressure and surface gravity for cool dwarf photospheres. This in turn will lead to much improved values for the fundamental parameters radius, luminosity and mass, for stars at the end of the main sequence.