A Three Body Solution for the DI Her System

Details A Three Body Solution for the DI Her System A Three Body Solution for the DI Her System

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ap%26ss.304..243h&link_type=abstract

Astrophysics and Space Science, Volume 304, Issue 1-4, pp. 243-246

Astronomy and Astrophysics

Astrophysics

3

Planetary Systems, Stars: Binaries: Eclipsing, Celestial Mechanics

Scientific paper

The DI Herculis system has been extensively studied over the past few decades because its observed rate of apsidal advance is less than a quarter of that which is expected from its physical and orbital properties. Work by Khaliullin et al. (1991) proposed that this slow rate of apsidal advance is a result of the presence of a third (stellar mass) body orbiting the system, however, observations by Guinan et al. (1994) severely restrict the orbital properties of such a solution. We show that a planetary mass object in a highly inclined orbit relative to the binary is capable of producing the observed apsidal motion, while remaining within the bounds of the most recent set of observations. A wide range of stable solutions are possible.

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