Revisiting the Anomalous Apsidal Motion of the Eccentric Eclipsing Binary DI Herculis

Details Revisiting the Anomalous Apsidal Motion of the Eccentric Eclipsing Binary DI Herculis Revisiting the Anomalous Apsidal Motion of the Eccentric Eclipsing Binary DI Herculis

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...203.1219m&link_type=abstract

American Astronomical Society Meeting 203, #12.19; Bulletin of the American Astronomical Society, Vol. 35, p.1224

Astronomy and Astrophysics

Astronomy

Scientific paper

In 1985, Guinan & Maloney presented the detailed analysis of the puzzling eclipsing binary system DI Herculis. This system is rare among main sequence stars in that its apsidal motion is dominated by the effects of General Relativity. The GR contribution to its theoretically predicted apsidal motion is 2.34 o/100 y., whereas the theoretically predicted classical contribution (due to tidal and rotational deformation of the component stars) is 1.93 o/100 y. The interesting fact is that the observed apsidal motion, determined from timings of the stars' mutual eclipses, is anomalously low: ˜1 o/100 y., well below the combined theoretical expectation of 4.27 o/100 y.
Since Rudkj\o bing's (1959) announcement of the special nature of DI Her, observers have been measuring light curves and radial velocity curves to determine the orbital parameters of the system and the stellar properties of its components. DI Her consists of two main sequence stars (B5V and B6V) in a 10.55 day eccentric orbit (e=0.489). Observations of times of minima reveal the system's apsidal motion, computed from the changing displacement of the secondary eclipse from the primary eclipse. Four decades of photoelectric measurements show that the observed apsidal motion remains below that predicted. Various explanations for this discrepancy have been offered, with the most promising involving the presence of a third component of the system. In a highly inclined orbit, the third body would diminish the rate of apsidal advance of the close pair. Adding photometry recently taken with the 0.8 m Four College Automatic Photoelectric Telescope, we present a new determination of the apsidal motion for DI Her. We also present the results from a new formalism for studying three-body interactions by Mardling in the DI Her system.
This research is supported by NSF/RUI grant AST00-71260, which we gratefully acknowledge.

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