Tau Scorpii

Tau Scorpii, Latinized from τ Scorpii, also named Paikauhale, is a star in the southern zodiac constellation of Scorpius. The apparent visual magnitude of Tau Scorpii is +2.8, which makes it among the brightest stars of the Scorpius constellation. Parallax measurements yield a distance estimate of roughly 470 light-years from Earth.

Nomenclature

τ Scorpii is the star's Bayer designation.
Tau Scorpii and Sigma Scorpii together bore the traditional name Al Niyat derived from the Arabic النياط al-niyāţ "the arteries" and referring to their position flanking the star Antares, the scorpion's heart, with Tau Scorpii being the star to the south.
Paikauhale is the Hawaiian name for Tau Scorpii. It forms a line of three stars with Hōkū-'ula and Au-haele. In the Hawaiian dictionary by Pukuʻi & Elbert, the word paikauhale is defined as to go gadding about from house to house. In another Hawaiian dictionary, paikauhale is defined as Vagabond owning no home; house-to-house wanderer.
In 2016, the IAU organized a Working Group on Star Names to catalog and standardize proper names for stars. The WGSN approved the name Paikauhale for this star on 10 August 2018 and it is now so included in the IAU Catalog of Star Names. The name Alniyat was given to Sigma Scorpii.
The indigenous Boorong people of northwestern Victoria saw this star as wives of Djuit.
In Chinese astronomy, 心宿, meaning Heart, refers to an asterism consisting of τ Scorpii, σ Scorpii and Antares. Consequently, the Chinese name for τ Scorpii itself is 心宿三, "the Third Star of Heart".

Description

Tau Scorpii is a B-type star with an early spectral classification of B0.2V. It has 15 times the Sun's mass and 6.4 times the radius of the Sun. It is radiating about 25,000 times the Sun's luminosity from its photosphere at an effective temperature of 28,860 K. This gives it the blue-white hue characteristic of B-type stars. As yet there is no evidence of a companion in orbit around τ Sco. It is a magnetic star whose surface magnetic field was mapped by means of Zeeman–Doppler imaging. Tau Scorpii is rotating relatively slowly with a period of 41 days.
This star is 5.22 million years old, being in the main sequence. Since it is more massive than the Sun, Tau Scorpii will evolve and exhaust its core hydrogen much faster. It is expected that in around 5.38 million years it will leave the main sequence, expanding to 10.9 times the Sun's radius, and in 6.4 million years, it will become a red supergiant with 750 times the radius of the Sun, comparable to Antares which is.
Waters et al. suggested that Tau Scorpii may be a rapidly rotating Be star that is being viewed pole-on. To explain its slow rotation, it has also been suggested that it is a blue straggler.
The spectrum of Tau Scorpii shows triply ionized oxygen that is being generated by X-rays and the Auger ionization effect. Observations with the ROSAT space telescope showed it has a higher energy X-ray spectrum than is usual for B0 V stars. Over the energy range, its X-ray luminosity is L_x = with a large L_x to L_bol ratio of log/L_bol = −6.53 from ASCA measurements. ROSAT measurements showed a log L_x/L_bol ≃ −5.93 for the range. The hard component of the X-ray spectrum from τ Sco as studied with XMM-Newton supports the presence of in-falling clumps of plasma in τ Sco.
Tau Scorpii star is a proper motion member of the Upper Scorpius subgroup of the
Scorpius–Centaurus OB association,
the nearest such co-moving association of massive stars to the Sun. The Upper Scorpius subgroup contains thousands of young stars with mean age 11 million years at average distance of 470 light years.