On the Li and Be tests for brown dwarfs

Details On the Li and Be tests for brown dwarfs On the Li and Be tests for brown dwarfs

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...413..364n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 413, no. 1, p. 364-367.

Astronomy and Astrophysics

Astrophysics

41

Brown Dwarf Stars, Metallicity, Stellar Interiors, Stellar Mass Ejection, Beryllium, Lithium, Stellar Evolution

Scientific paper

We present the results of stellar evolution calculations which show quantitatively how the measured abundances of Li and Be in low-mass stellar objects can be used to discriminate between brown dwarfs and low-mass main-sequence stars. The evolution of B, although less useful, is also studied. We define a transition mass range, below which at least 50 percent of the light element remains at the end of nuclear burning, and above which no more than 10 percent remains. We find that the transition mass range for Li burning is 0.059-0.062 solar mass, while for Be the range is 0.075-0.077 solar mass. Using these results, we then examine the factors (e.g., age and luminosity) that affect our ability to identify low-luminosity objects as brown dwarfs. In particular, we show that the Li test would be well suited for brown dwarf candidates located in nearby open clusters with ages in the range of 2 x 10 exp 8 to 5 x 10 exp 8 yr.

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