Masses and Multiplicity of Nearby Free- floating Methane and L Dwarfs

Details Masses and Multiplicity of Nearby Free- floating Methane and L Dwarfs Masses and Multiplicity of Nearby Free- floating Methane and L Dwarfs

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8720b&link_type=abstract

HST Proposal ID #8720

Computer Science

Hst Proposal Id #8720 Cool Stars

Scientific paper

Brown dwarfs never stabilize themselves on the hydrogen main sequence, thus there is an ambiguity between the temperature or luminosity of a given object and its mass or age. In order to test the mass-luminosity relations of {still uncertain} evolutionary models, a direct dynamical determination of mass is required. As a first step towards a dynamical mass estimate for brown dwarfs, we have compiled a sample of 50 very-low-mass objects {M<=0.08M_sun} in the solar neighborhood {distances 5 pc to 30 pc} with spectral types of L0 and later {including several dwarfs with Methane absorption bands in their atmospheres}. Using WFPC2, we propose to observe these objects in two filter bands with the aim to identify close companions, measure their colors, and to obtain first epoch data of the newly discovered binaries. We show that the closest binary brown dwarfs we can resolve will have orbital periods between 3 and 10 yr. Hence, within a few years we should be able to very accurately pin down masses for brown dwarfs and to calibrate evolutionary tracks. Binary properties like multiplicity, distribution of binary separations and brightness ratios hold clues on the origin of free-floating brown dwarf binaries. Our program will be an important step towards a better understanding of the still elusive class of brown dwarfs.

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