The Structure of the M Dwarf Stars. I.

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Abstract

The problem of the internal structure of the middle and late M dwarf stars is considered, and the discrepancy between theory and observation that had been found by Osterbrock for these stars is reexamined. A rediscussion of the observations that relate to the masses, luminosities, and radii for the stars whose spectral types range from M4 V to M8 V is carried out on the basis of what are believed to be the best and most recent data; and revised values and probable errors for these observational quantities are determined. The evidence is found to indicate rather strongly that the bolometric corrections that are usually quoted in the literature should be reduced by at least 0.3 or 0.4 mag. for the stars of spectral type M4 V and by correspondingly larger values for the still later spectral types. Some indication is also found that the effective temperatures of the middle and late M dwarfs are actually higher than the values usually quoted. These suggested corrections act to reduce significantly the discrepancy between Osterbrock's theory and the observations and lend support to the view that the middle and late M dwarfs are completely convective insofar as their interiors are concerned.

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