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Period Changes of the Algol System SZ Herculis

Published online by Cambridge University Press:  23 April 2012

J. W. Lee ,
C.-U. Lee ,
S.-L. Kim ,
H.-I. Kim ,
J.-H. Park  and
T. C. Hinse
J. W. Lee
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea email: [email protected]
C.-U. Lee
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea email: [email protected]
S.-L. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea email: [email protected]
H.-I. Kim
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea email: [email protected]
J.-H. Park
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea email: [email protected]
T. C. Hinse
Affiliation:
Korea Astronomy and Space Science Institute, Daejeon 305-348, Korea email: [email protected]
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Abstract

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New CCD photometric observations of SZ Her were obtained between February and May 2008. More than 1,100 times of minimum light spanning more than one century were used for the period analysis. We find that the orbital period of SZ Her has varied due to a combination of two periodic variations, with cycle lengths of P3 = 85.8 yr and P4 = 42.5 yr and semi-amplitudes of K3 = 0.013 days and K4 = 0.007 days, respectively. The most reasonable explanation for them is a pair of light-time-travel (LTT) effects driven by the existence of two M-type companions with minimum masses of M3 = 0.22 M⊙ and M4 = 0.19 M⊙, located at nearly 2:1 mean motion resonance. Then, SZ Her is a quadruple system and the 3rd and 4th components would stay in the stable orbital resonance.

Keywords

binaries: closebinaries: eclipsingstars: individual (SZ Herculis)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 313 - 314
Copyright
Copyright © International Astronomical Union 2012

References

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Szekely, P. 2003, IBVS, 5467, 1Google Scholar