A period investigation of the overcontact binary system V417 Aquilae
Abstract
A detailed orbital period investigation of the short-period (P=0fd 37) W UMa type star, V417 Aql, is presented based on the analysis of its O-C data. It is shown that the period change of the binary system is continuous. A periodic variation, with a period of 42.4 years and an amplitude of 0fd 0130, is found superimposed on a long-term period decrease (dP/dt=-5.50x10-8 days/year). The period oscillation can be explained either by the light-time effect via the presence of an unseen third body or by magnetic activity cycles of the components. V417 Aql is a W-type overcontact binary system with a low mass ratio of q=0.36. The long-term period variation is in agreement with the conclusion of Qian (\cite{Qian01}b) that a low-mass ratio W-type system usually shows a secular period decrease. This suggests that V417 Aql is on the AML-controlled stage of the evolutionary scheme proposed by Qian (\cite{Qian01}b). Meanwhile, the light-curve paradox encountered by TRO theory is discussed.
- Publication:
-
Astronomy and Astrophysics
- Pub Date:
- March 2003
- DOI:
- 10.1051/0004-6361:20030018
- Bibcode:
- 2003A&A...400..649Q
- Keywords:
-
- stars: binaries: close;
- stars: binaries: eclipsing;
- stars: individual: V417 Aql;
- stars: evolution