Spectrum Synthesis of Hot Water in Sunspots and Selected Cool Stars

Details Spectrum Synthesis of Hot Water in Sunspots and Selected Cool Stars Spectrum Synthesis of Hot Water in Sunspots and Selected Cool Stars

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...189.8103c&link_type=abstract

American Astronomical Society, 189th AAS Meeting, #81.03; Bulletin of the American Astronomical Society, Vol. 28, p.1382

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Scientific paper

Very recently, Partridge and Schwenke (1996) completed an elaborate theoretical computation of the potential energy surface and dipole moment function for H2O. They have used their results to predict the positions and strengths of nearly 308 million (1) H(1) H(16) O lines. This line tabulation is the most complete now available. It extends to sufficiently high excitations that the spectra of M-stars may be modelled with greater accuracy than ever before provided the predicted line parameters of Partridge and Schwenke are themselves accurate. We have computed synthetic sunspot spectra using the Partridge and Schwenke H2O line list and the sunspot umbral models of Maltby et al (1986). In this display, we compare these synthetic spectra with published high resolution sunspot atlases. We demonstrate the extent to which the new H2O line list successfully predicts the sunspot H2O spectrum and suggest where improvements are necessary. Using the new H2O tabulation, we also illustrate the extent to which hot stellar H2O blankets the H, K and L passbands for selected K and M-star model atmospheres.

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