M Dwarfs, L Dwarfs, T Dwarfs and Subdwarfs: Ψ(M) at and below the Hydrogen-Burning Limit

Details M Dwarfs, L Dwarfs, T Dwarfs and Subdwarfs: Ψ(M) at and below the Hydrogen-Burning Limit M Dwarfs, L Dwarfs, T Dwarfs and Subdwarfs: Ψ(M) at and below the Hydrogen-Burning Limit

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999sf99.proc..327r&link_type=abstract

Star Formation 1999, Proceedings of Star Formation 1999, held in Nagoya, Japan, June 21 - 25, 1999, Editor: T. Nakamoto, Nobeyam

Computer Science

1

Scientific paper

Eighty percent of the stars within the immediate Solar Neighbourhood are M dwarfs, and low mass stars make a correspondingly large contribution to the stellar mass budget. Until recently, the mass density due to substellar mass brown dwarfs was a matter for speculation, but results from the new generation of near-infrared sky surveys (DENIS and 2MASS), supplemented by deeper optical/far-red surveys (POSS II and, most recently, SDSS) have revolutionised this area of research. I review these new observational discoveries and consider their interpretation in the light of recent theoretical models. I consider the conclusions which can be drawn regarding the likely form of the stellar/sub-stellar mass function for the Galactic disk, and compare those results against recent determinations of the mass function in the Galactic halo.

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