2013/10/29 by Francis C. Fekel, Gregory W. Henry, James R. Sowell · 1 citation
Physics and Astronomy · #Stellar, planetary, and galactic studies #Astrophysics and Star Formation Studies #Astronomy and Astrophysical Research #Physics #Photometry (optics) #Astrophysics #Orbital eccentricity #Orbital period #Proper motion #Orbital elements #Binary number #Light curve #Primary (astronomy) #Eccentricity (behavior) #Radial velocity #Astronomy #Wavelength #Planet #Stars #Optics
paper · doi:10.1088/0004-6256/146/6/146
openalex publication_date 2013/10/29 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We have obtained red-wavelength spectroscopy and Johnson B and V differential photoelectric photometry of the eclipsing binary VV Crv = HR 4821. The system is the secondary of the common proper motion double star ADS 8627, which has a separation of 5 2. VV Crv has an orbital period of 3.144536 days and a low but non-zero eccentricity of 0.085. With the Wilson–Devinney program we have determined a simultaneous solution of our spectroscopic and photometric observations. Those orbital elements produce masses of M 1 = 1.978 ± 0.010 M ☉ and M 2 = 1.513 ± 0.008 M ☉ , and radii of R 1 = 3.375 ± 0.010 R ☉ and R 2 = 1.650 ± 0.008 R ☉ for the primary and secondary, respectively. The effective temperatures of the two components are 6500 K (fixed) and 6638 K, so the star we call the primary is the more massive but cooler and larger component. A comparison with evolutionary tracks indicates that the components are metal rich with [Fe/H] = 0.3, and the system has an age of 1.2 Gyr. The primary is near the end of its main-sequence lifetime and is rotating significantly faster than its pseudosynchronous velocity. The secondary is still well ensconced on the main sequence and is rotating more slowly than its pseudosynchronous rate.