V752 Centauri

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{{Starbox detail | no_heading=1 | source = | component1=Primary | mass = 1.31 ± 0.07 | radius = 1.30 ± 0.02 | luminosity = 2.00 ± 0.07} | gravity = | temperature = 5,955 ± 77 | metal_fe = | rotational_velocity = | age_gyr = | component2=Secondary | mass2 = 0.39 ± 0.02 | radius2 = 0.77 ± 0.01 | temperature2 = 6,221 ± 81 | luminosity2 = 0.75 ± 0.03 }} V752 Centauri (HD 101799) is multiple star system and variable star in the constellation of Centaurus. An eclipsing binary, its apparent magnitude has a maximum of 9.10, dimming to 9.66 during primary eclipse and 9.61 during secondary eclipse. Its variability was discovered by Howard Bond in 1970. From parallax measurements by the Gaia spacecraft, the system is located at a distance of from Earth. V752 Centauri is a contact binary of the W Ursae Majoris type, composed of two F-type stars with a combined spectral type of F7/G0(V). Individually, the components have been classified as F8 + F5, and F8 + F7.5. With effective temperatures of 5,955 and 6,221 K, the system is classified as a W Ursae Majoris variable of subtype W, where the secondary star is hotter than the primary; for this reason, the primary eclipses are caused by the occultation of the secondary star. The system has an orbital period of only 0.3702 days and a separation of 2.59 solar radii. The orbit is inclined by 82° in relation to the plane of the sky.…

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