2007/07/31 by J. L. Christiansen, Jessie L. Christiansen, A. Derekas +7 · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.12338.x
7 pages, 6 figures, 2 tables, for submission to MNRAS, v2: paper size change, small typographical changes to abstract
arxiv created 2007/07/31 · openalex publication_date 2007/10/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
We report the discovery of the first high-amplitude δ Scuti star in an eclipsing binary, which we have designated UNSW-V-500. The system is an Algol-type semi-detached eclipsing binary of maximum brightness V= 12.52 mag. A best-fitting solution to the binary light curve and two radial velocity curves is derived using the Wilson–Devinney code. We identify a late-A spectral-type primary component of mass 1.49 ± 0.02 M⊙ and a late-K spectral-type secondary of mass 0.33 ± 0.02 M⊙, with an inclination of , and a period of 5.350 4751 ± 0.000 0006 d. A Fourier analysis of the residuals from this solution is performed using period04 to investigate the δ Scuti pulsations. We detect a single pulsation frequency of f1= 13.621 ± 0.015 cd−1, and it appears that this is the first overtone radial mode frequency. This system provides the first opportunity to measure the dynamical mass for a star of this variable type; previously, masses have been derived from stellar evolution and pulsation models.