On the luminosity ratio of pre-main sequence binaries

Details On the luminosity ratio of pre-main sequence binaries On the luminosity ratio of pre-main sequence binaries

Oct 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...338..452m&link_type=abstract

Astronomy and Astrophysics, v.338, p.452-454 (1998)

Astronomy and Astrophysics

Astrophysics

12

Binaries: Visual, Stars: Pre-Main-Sequence, Stars: Low-Mass, Brown Dwarfs

Scientific paper

Assuming random pairing of single stars from the same fundamental IMF as a good scenario for pre-main sequence binary formation, we show how to derive the mass ratio distribution and the fundamental IMF from the observational luminosity ratio distribution, taking into account pre-main sequence evolution. We also determine how the detectability of a brown dwarf as a companion relates to its own mass, the mass of the primary, and the age of the system. Our calculations suggest that for a particular mass of a brown dwarf companion, there is a ``best age'' for detection, namely when the brown dwarf is in its deuterium burning phase. Clusters with ages 10(6) to 10(7) years would be most favorable to catch brown dwarfs at their ``best age''.

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