Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..240..130c&link_type=abstract
Binary Stars as Critical Tools and Tests in Contemporary Astrophysics, International Astronomical Union. Symposium no. 240, he
Astronomy and Astrophysics
Astrophysics
1
Scientific paper
Theta 1 Ori E = ADS 4186 E = NSV 2291 , the fifth brightest star in the Orion Trapezium, was reported to be a double-lined spectroscopic binary by Costero et al. 2006 (IAUC 8669). In this paper we present the derived orbital elements of the binary system and physical parameters of its members. The velocity curve of each component was derived from 61 Echelle spectra in which the absorption systems are not blended. The radial velocities were obtained by cross-correlating these spectra with those of two reference stars with well-measured radial velocities, in the 5120 -"5515 Å spectral range. The binary components are nearly identical, their composite spectral type being around G0IV. The Li I 6708 Å absorption line is strong and the Ca II K line is in emission inboth stars, indicative of their pre-main sequence evolutionary stage. The orbit is circular (e <10^-3). The orbital period and systemic velocity are 9.896 ± 0.001 d and 32.4 ± 1.0 km/s.The semi-amplitude of both components is 85.7±3.0 km/s. From the published K magnitude for the object and a suitable pre-main sequence stellar evolution model, we find the bolometric luminosity, radius and mass of each component to be, respectively, 89, 8.4 and 4.0 (in solar units), if the stars are identical to each other. Based on the latter values, the orbital inclination is about 59°, while the minimum Inclination for grazing eclipses to occur is 65°. Hence, no observable eclipses in this binary are expected.
Costero Rafael
Echevarria J. J.
Poveda Arcadio
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