Orbital Period Studies of Two Algol-Type Eclipsing Binary Systems: TY Pegasi and X Trianguli

Details Orbital Period Studies of Two Algol-Type Eclipsing Binary Systems: TY Pegasi and X Trianguli Orbital Period Studies of Two Algol-Type Eclipsing Binary Systems: TY Pegasi and X Trianguli

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002pasp..114..650q&link_type=abstract

The Publications of the Astronomical Society of the Pacific, Volume 114, Issue 796, pp. 650-655.

Astronomy and Astrophysics

Astronomy

7

Stars: Binaries: Close, Stars: Individual (Ty Pegasi), Stars: Individual (X Trianguli), Stars: Mass Loss

Scientific paper

O-C curves of two EA-type eclipsing binaries, TY Peg and X Tri, are formed and studied in detail based on all available times of light minimum. For TY Peg, it was discovered that the general trend of the O-C curve showed a downward parabolic variation, which indicates a secular period decrease with rate at dP/dt=-1.16×10-6 days yr-1. When the secular decrease is removed from the O-C curve, the residuals can be described by several linear ephemerides, suggesting several sudden period jumps. For the other one, X Tri, it is found that the general O-C trend also indicates a secular period decrease (dP/dt=-1.42×10-7 days yr-1), and several irregular period jumps are found to superpose on the long-time period decrease. This kind of period change, irregular sudden jumps superposed on secular decrease, is typical for many other Algol-type binary systems such as TU Her, UU And, Z Per, Y Psc, BO Mon, FH Ori, RT Per, and TX UMa. The period changes of these systems may be caused by orbital angular momentum loss via variable magnetic coupling and gravity coupling between the components.

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