AAVSO: American Association of Variable Star Observers

New Observations and Analysis of zeta Phoenicis (Abstract)

Volume 45 number 2 (2017)

Coen van Antwerpen
Coki Observatory, 8 Carman Close, Hillbank, SA 5112, Australia; coenva15@gmail.com
Tex Moon
Centauri Observatory, 14 Ada St, Scottsdale, TAS 7260, Australia; texmoon0@gmail.com


(Abstract only) From new and published photometry of the eclipsing binary zeta Phe (HR 338) a period of 1.66977220(3) days was determined and a new epoch of HJD 2432500.021511 selected. Using the 60+ years of photometry, published radial velocities, and new values for the period and epoch, the physical characteristics of the zeta Phe system were modeled using a software package called phoebe. Of note, the masses of the B6V and B9V components were determined to be 3.75 and 2.35 M, somewhat less than previous determinations. The period of apsidal motion of zeta Phe’s eccentric orbit was calculated to be 53.7 ± 0.3 years, indicating that one full cycle has been completed since photoelectric measurements of this star were first undertaken in 1950.