The presented analysis of α CrB is based on the Ebbighausen (1976) spectroscopic observations of the primary component, on the McDonald Reticon observations of the secondary, and on the Kron-Gordon (1953) photometric observations at 0.72 μm. The primary component, with mass 2.6 M_sun; and spectral type A0, lies about 0.4 mag above the zero-age main sequence, while the secondary, with mass 0.92 M_sun;, has a radiative flux corresponding to a type near G5, and must lie close to the ZAMS. The system is unique among analyzed main-sequence systems with respect to its small mass ratio and large magnitude difference between the components.
No takes yet. Share an insight, caveat, or question.
Tomkin et al. (1986) studied this question.