The third body in the eclipsing system RR Lyn |
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| Authors: | Kh F Khaliullin A I Khaliullina |
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| Institution: | (1) Sternberg Astronomical Institute, Universitetskii pr. 13, Moscow, 119899, Russia |
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| Abstract: | Based on 70 years of published photoelectric observations, we have detected quasi-periodic cophased oscillations of the times of the primary and secondary minima of RR Lyn, one of the brightest and nearest eclipsing binaries in the northern sky ( $V = 5\mathop m\limits_. 54$ ; r=74 pc). Approximating these oscillations using the light equation yields estimates of the orbital parameters of the third body in the system and imposes constraints on its mass, M 3. In the most probable case when the orbits of the eclipsing and triple systems are coplanar, M 3=1.10±0.02M ⊙, and the semimajor axis of the orbit A 3=17.4±3.5 AU, with a substantial eccentricity, e 3=0.96±0.02. We have carried out a detailed study of the apsidal rotation of this eclipsing and now multiple system, which was suggested by Koch as a test of general relativity as far back as 1973. Our high-precision W BV R photoelectric photometry $(\sigma _{obs} \cong 0\mathop m\limits_. 0032)$ has removed some contradictions. At the same time, the proximity of the longitude of periastron ω 180°; the close correlation between the jointly estimated values of ω, e and the limb-darkening coefficients for the component disks, u 1 and u 2; and microfluctuations in the brightnesses of the stars prevent determination of the rate of rotation of the elliptical orbit in the system, even using the most accurate measurements. |
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