HU Tauri

rdf:langString HU Tauri

rdf:langString −0.019

rdf:langString

rdf:langString B8V + G2IV

rdf:langString Primary

rdf:langString Secondary

rdf:langString J2000.0

rdf:langString −7.198

rdf:langString −12.899

rdf:langString −2.3

rdf:langString Semi-detached Algol variable

rdf:langString HU Tauri is a tight binary star system in the equatorial constellation of Taurus. It is an eclipsing binary, which means that the member stars periodically eclipse each other every 2.056 days. They have a combined apparent visual magnitude of 5.85, which is bright enough to be dimly visible to the naked eye. During the primary eclipse, the magnitude drops to 6.68, while the secondary eclipse decreases the magnitude to 5.91. The distance to this system, based on parallax measurements, is approximately 414 light years. The variable nature of this system was reported by and R. Knigge in 1960. In 1963, Strohmeier found a period of 2.056297 days, and and associates derived orbital elements for a single-lined spectroscopic binary in 1967. A light curve for the system was assembled by O. Tümer and in 1979. and M. B. K. Sarma in 1980 noted asymmetries in the light curve near the primary eclipse, which suggested gas streams are partially obscuring the light from the primary component. This is a semidetached binary system with an orbital period of 2.0563056 days in an essentially circular orbit. The primary component is presently a B-type main-sequence star with a stellar classification of B8V. It has 4.4 times the mass and 2.6 times the radius of the Sun. The primary eclipse is an occultation in which the secondary completely covers the primary. The cooler and larger secondary star is over-luminous for its mass, indicating that it has evolved away from the main sequence, and is filling its Roche lobe. The spectrum of the system suggests that the secondary is undergoing mass loss, with a gas stream transferring matter to the primary.