On the mass-radius relation of late M dwarfs

Details On the mass-radius relation of late M dwarfs On the mass-radius relation of late M dwarfs

Sep 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990aj....100..825c&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 100, Sept. 1990, p. 825-829.

Astronomy and Astrophysics

Astronomy

56

Dwarf Stars, M Stars, Radii, Stellar Mass, Astronomical Photometry, Cataclysmic Variables, Infrared Photometry, Mass To Light Ratios, Stellar Luminosity

Scientific paper

An attempt is made to rederive an empirical mass-radius relation for main-sequence stars less massive than 0.5 solar mass. Near-infrared photometry (JHK bands) was obtained on about 40 nearby (all with greater than 0.04 arcsec) low-mass taken from the Gliese catalogs. From these data and from previously published UBVRI magnitudes, effective temperatures are determined in the standard manner, by fitting blackbody energy distributions to the observed fluxes while allowing for line and band blocking below 1 micron. Together with the known distances, these temperatures and fluxes allow estimates of the radii and luminosities of these stars. Invoking a theoretical mass-luminosity relation, the masses of the stars can then be derived. A comparison of the resultant empirical mass-radius relation with a recent theoretical relation shows that the discrepancy is now about 10 percent, significantly better than the 20-25 percent obtained a decade ago.

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