Interferometric astrometry of the detached white dwarf-M dwarf binary Feige 24 using HST Fine Guidance Sensor 3: White dwarf radius and component mass estimates
Gf. Benedict et al., Interferometric astrometry of the detached white dwarf-M dwarf binary Feige 24 using HST Fine Guidance Sensor 3: White dwarf radius and component mass estimates, ASTRONOM J, 119(5), 2000, pp. 2382-2390
With Hubble Space Telescope Fine Guidance Sensor 3 we have determined a par
allax for the white dwarf-M dwarf interacting binary, Feige 24. The white d
warf (DA) component has an effective temperature T-eff similar to 56,000 K.
A weighted average with past parallax determinations (pi(abs) = 14.6 +/- 0
.4 mas) narrows the range of possible radius values, compared with past est
imates. We obtain R-DA = 0.0185 +/- 0.0008 R. with uncertainty in the tempe
rature and bolometric correction the dominant contributors to the error. Fi
ne Guidance Sensor 3 photometry provides a light curve entirely consistent
with reflection effects. A recently refined model mass-luminosity relation
for low-mass stars provides a mass estimate for the M dwarf companion, M-dM
= 0.37 +/- 0.20 M., where the mass range is due to metallicity and age unc
ertainties. Radial velocities from Vennes and Thorstensen provide a mass ra
tio from which we obtain M-DA = 0.49(-0.05)(+0.19) M.. Independently, our r
adius and recent log g determinations yield 0.44 M. < M-DA < 0.47 M.. In ea
ch case, the minimum DA mass is that derived by Vennes & Thorstensen from t
heir radial velocities and Keplerian circular orbits with i less than or eq
ual to 90 degrees. Locating Feige 24 on an (M, R)plane suggests a carbon co
re. Our radius and these mass estimates yield a value of gamma(gray) incons
istent with that derived by Vennes & Thorstensen. We speculate on the natur
e of a third component whose existence would resolve the discrepancy.