Pi Scorpii system

Pi Scorpii is a triple star system.

The main components of this system form an eclipsing binary of the Beta Lyrae type. Both its members are hot, B-type main sequence stars with a blue-white hue. They display an ellipsoidal variation of 0.03 in magnitude. The two stars are rotating rapidly, with projected rotational velocities of 108 and 87 km s−1, respectively. Their orbital period is 1.571 days and they are on a very close circular orbit.

The binary system is orbited by a smaller, more distant companion. This component is separated from the pair by at least 7000 AU.

The Pi Scorpii system is a kinematic member of the Upper Scorpius subgroup of the Scorpius-Centaurus Association, a group of thousands of young stars with mean age 11 million years at distance 470 light years (145 parsecs). An analysis of the HR diagram position for the primary star Pi Scorpii A estimates its effective temperature to be 25,230 K, consistent with an isochronal age of 12-14 million years.