Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26as...47..319b&link_type=abstract
Astronomy and Astrophysics Supplement, Vol. 47, P. 319, 1982
Astronomy and Astrophysics
Astrophysics
2
Scientific paper
The Scuti type star V644 Her, first known as a spectroscopic binary, was observed from 2 March to 11 November 1980 with the CO RAVEL photoelectric spectrometer at the Observatoire de Haute-Provence. In order to correct the observed radial velocities for the orbital motion, a mean value of each night's measurements has been considered, with the corresponding epoch, and new spectroscopic elements have been computed. Taking into account previous observations, an accurate period has been determined:
P = 11.858592 ± 0.000040 days.
The other orbital elements, obtained with CORAVEL results only, are the following:
K = 27.44 ± 0.30 km s-1
V0 = - 0.59 ± 0.19 km s-1
e = 0.3650 ± 0.0093
ω = 267°72 ± 1°78
T0 = 2444553.759 ± 0.048 JD
TN = 2444555.439 ± 0.034 JD
a sin i = 4166000 ± 62000 km
f(M) = 0.02054 ± 0.00092 Msun
A new calculation of Harper's (1931-32) and Shajn-Melnikov's (1934-35) orbits confirms a significant difference in the V0 mean radial velocities of the system certainly due to a zero difference in the measurements, but shows no evident apsidal motion. Assuming for this young disk variable an absolute magnitude of MV = 2.0, which is consistent with an F2IV spectral type, and a mass of about 1.5Msun, we find the secondary component to be cooler than an F6-8V star. The system is separated, with a distance of 30 Rsun between the two components, and an inclination greater than 30°. Its distance from us is about 6&76 or 72-83 pc, depending whether or not we take the brightness of the secondary component into account.
Bardin Cl.
Imbert M.
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