Beta Crucis - Properties

Properties

Beta Crucis is believed to be the hottest first-magnitude star, with an apparent visual magnitude of 1.25. Based on parallax measurements, it is located at a distance of 280 ly (86 pc) from the Earth. In 1957, German astronomer Wulff-Dieter Heintz discovered that it is a spectroscopic binary with components that are too close together to resolve with a telescope. The pair orbit each other every 5 years with an estimated separation that varies from 5.4 to 12.0 Astronomical Units. The system is only 8 to 11 million years old.

The primary, Beta Crucis A, is a massive star with about 16 times the Sun's mass. The projected rotational velocity of this star is about 35 km s–1. However, the orbital plane of the pair is only about 10°, which probably means the inclination of the star's pole is also likely to be low. This suggests that the azimuthal rotational velocity is quite high, at about 120 km s–1. With a radius of about 8.4 times the radius of the Sun, this would mean the star has a rotational period of only about 3.6 days.

Beta Crucis A is a known Beta Cephei variable, although with an effective temperature of about 27,000 K it is at the high end of the instability strip where such stars are found. It has three different periods of pulsation, none of which are radial. All of the pulsation periods are in the range of 4.03–4.59 hours. The star has a stellar classification of B0.5 III, with the luminosity class of 'III' indicating that this is a giant star that has exhausted the supply of hydrogen at its core. The high temperature of the star's outer envelope is what gives the star the blue-white hue that is characteristic of B-type stars. It is generating a strong stellar wind and is probably losing about 10–8 times the mass of the Sun per year, or the equivalent of the mass of the Sun every 100 million years. The wind is leaving the system with a velocity of 2,000 km s–1 or more.

The secondary companion in this system may be a main sequence star with a stellar class of B2. In 2007, a third companion was announced, which may be a low mass, pre-main sequence star. The X-ray emission from this star was detected using the Chandra X-ray Observatory. Two other stars, located at angular separations of 44 and 370 arcseconds, are likely optical companions that are not physically associated with the system. The Beta Crucis system may be a member of the Lower Centaurus-Crux sub-group of the Scorpius-Centaurus Association. This is a stellar association of stars that share a common origin.