Publ. Astron. Soc. Pac., 117, 173-188 (2005/February-0)
The prospects for finding brown dwarfs in eclipsing binary systems and measuring brown dwarf properties.
PINFIELD D.J., JONES H.R.A. and STEELE I.A.
Abstract (from CDS):
We present the results of a simulation to investigate the prospects of measuring mass, age, radius, metallicity, and luminosity data for brown dwarfs in fully eclipsing binary systems around dwarf spectral types from late K to early M that could be identified by ultra-wide-field transit surveys such as SuperWASP. These surveys will monitor approximately a million K and M dwarfs with|b|>20° (where blending of sources is not a significant problem) at a level sufficient to detect transits of low-luminosity companions. We look at the current observational evidence for such systems and suggest that ∼1% of late K and early-to-mid M dwarfs could have a very close (∼0.02 AU) brown dwarf companion. With this assumption, and using SuperWASP as an example, our simulation predicts that ∼400 brown dwarfs in fully eclipsing binary systems could be discovered. All of these eclipsing binaries could yield accurate brown dwarf mass and radius measurements from radial velocity and follow-up light curve measurements. By inferring the brown dwarf effective temperature distribution, assuming a uniform age spread and an α=0.5 companion brown dwarf mass function, the simulation estimates that brown dwarf brightness could also be measurable (at the 10% level) for ∼60 of these binary systems from near-infrared follow-up light curves of the secondary eclipse. We consider irradiation of these brown dwarfs by their primary stars and conclude that it would be below the 10% level for ∼70% of them. This means that in these cases, the measured brown dwarf brightnesses should essentially be the same as those of free-floating counterparts. The predicted age distribution of the primaries is dominated by young systems, and ∼20 binaries could be younger than 1 Gyr. Irradiation will be below the 10% level for ∼80% of these. We suggest that many of these young binary systems will be members of ``kinematic moving groups'', allowing their ages to be accurately constrained.
Stars: Low-Mass, Brown Dwarfs - Stars: Fundamental Parameters - Stars: Binaries: Eclipsing - Techniques: Photometric
In table 2 Fomalhault is a misprint for Fomalhaut
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