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Title:
A Three Body Solution for the DI Her System
Authors:
Hsuan, Keith; Mardling, Rosemary A.
Affiliation:
AA(Centre for Stellar and Planetary Astrophysics, Monash University), AB(Centre for Stellar and Planetary Astrophysics, Monash University)
Publication:
Astrophysics and Space Science, Volume 304, Issue 1-4, pp. 243-246 (Ap&SS Homepage)
Publication Date:
08/2006
Origin:
SPRINGER
Keywords:
Planetary systems, Stars: binaries: eclipsing, Celestial mechanics
DOI:
10.1007/s10509-006-9121-0
Bibliographic Code:
2006Ap&SS.304..243H

Abstract

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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