ABSOLUTE PROPERTIES OF THE ECLIPSING BINARY VV CORVI

作者：Fekel Francis C^*; Henry Gregory W; Sowell James R

来源：Astronomical Journal, 2013, 146(6): 146.

DOI：10.1088/0004-6256/146/6/146

• binaries: close
• binaries: eclipsing
• binaries: spectroscopic
• stars: individual (VV Crv)

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-circle dot and M-2 = 1.513 +/- 0.008 M-circle dot, and radii of R-1 = 3.375 +/- 0.010 R-circle dot and R-2 = 1.650 +/- 0.008 R-circle dot 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.

• 出版日期2013-12