Psi Centauri
Psi Centauri is a binary star system in the southern constellation of Centaurus. Its name is a Bayer designation that is Latinized from ψ Centauri, and abbreviated Psi Cen or ψ Cen. This system is visible to the naked eye as a point of light with a baseline apparent visual magnitude of +4.05. The distance to this system is 250 light years based on parallax. The radial velocity is poorly constrained, but it appears to be slowly drifting away from the Sun at the rate of +2 km/s.
This is a detached eclipsing binary system with the secondary eclipse being total. The pair are orbiting each other with a period of 38.81 days and an eccentricity of 0.55.The brightness of the system dips by 0.28 and 0.16 magnitude during the two eclipses per orbit. The system displays an infrared excess at a wavelength of 60 μm, indicating the presence of a circumstellar debris disk with a temperature of 120 K, orbiting at a distance of 64 AU.
The pair have a combined stellar classification of A0 IV, matching a white-hued A-type subgiant. The two components appear to be at different evolutionary stages. Both have high rotation rates, with projected rotational velocities over 120 km/s. The primary has 3.814 times the Sun's radius while the secondary is 1.896 times. The primary showed evidence of pulsational behavior with 1.996 and 5.127 cycles per day, which suggests it is a slowly pulsating B star. But this remains unconfirmed as of 2017, and the finding may instead be the result of instrumental error.