Analysis of Keck High Resolution Spectra of VB10

Details Analysis of Keck High Resolution Spectra of VB10 Analysis of Keck High Resolution Spectra of VB10

1996-06-24

arxiv.org/abs/astro-ph/9606150v1

Astronomy and Astrophysics

Astrophysics

8 pages, latex, MNRAS style, figures not included, full text plus figures available at http://brian.la.asu.edu/ or at ftp://

Scientific paper

We use a preliminary version of our ``NextGen'' grid of cool star model atmospheres to compute synthetic line profiles which fit high resolution Keck spectra of the cool M~dwarf VB10 satisfactorily well. We show that the parameters derived from the Keck data are consistent with the parameters derived from lower resolution spectra with larger wavelength coverage. We discuss the treatment of van der Waals broadening in cool, molecular (mostly ${\rm H_2}$) dominated stellar atmospheres. The line profiles are dominated by van der Waals pressure broadening and are a sensitive indicator for the gravity and metallicity. Therefore, the high-resolution Keck spectra are useful for determining the parameters of M dwarfs. There is some ambiguity between the metallicity and gravity. For VB10, we find from the high-resolution spectra that $ 5.0 < \log(g) < 5.5$ and $0 < \left[\case{{\rm M}}{{\rm H}}\right] < +0.5$ for an adopted fixed effective temperature of 2700~K (Schweitzer, 1995), which is consistent with recent interior calculations (Baraffe etal, 1995).

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