Lambda Tauri (λ Tau, λ Tauri) is a triple star system in the constellation Taurus. In the Calendarium of Al Achsasi Al Mouakket, this star was designated Sadr al Tauri, which was translated into Latin as Pectus Tauri, meaning "the bull chest". In 1848, the light from this system was found to vary periodically and it was determined to be an eclipsing binary system—the third such discovered. The components of this system have a combined apparent visual magnitude of +3.37 at its brightest, making it one of the brighter members of the constellation. Based upon parallax measurements from the Hipparcos mission, the distance to this system is approximately . System The inner pair of this triple star system, Lambda Tauri AB, orbit around each other with a period of 3.95 days and a low eccentricity of about 0.025. Their orbital plane is inclined by around 76° to the line of sight from the Earth, so it is being viewed from nearly edge on and the two stars form an Algol-like eclipsing binary system. The combined brightness of the pair varies from magnitude +3.37 to +3.91 as first one star and then the other pass in front of its companion. The primary member, λ Tau A, undergoes a decrease of in magnitude during an eclipse, while the secondary component, λ Tau B, decreases by 0.09–0.10 in magnitude. The mean physical separation between these two stars is estimated at 21.91 times the radius of the Sun, or . The primary component has a stellar classification of B3 V, making this a massive B-type main sequence star. It has over seven times the mass of the Sun and 6.4 times the Sun's radius. This star is the brightest member of the system, radiating about 5,801 times the luminosity of the Sun from its outer envelope at an effective temperature of , which gives it a blue-white hue common to the B-type stars. Lambda Tauri A is rotating rapidly with a projected rotational velocity of . It, along with δ Librae, were the first stars on which rotational line broadening was observed, by Frank Schlesinger in 1909. The third component, λ Tau C, is orbiting the inner pair over a 33.025 day period with an eccentricity of roughly 0.15. The orbital plane of this component is nearly coplanar with the orbit of Lambda Tauri AB, differing by no more than 7°. It has about