Mu1 Scorpii is aneclipsing binary of theBeta Lyrae type. Discovered to be aspectroscopic binary bySolon Irving Bailey in 1896, it was only the third such eclipsing pair to be discovered. This is asemidetached binary system where the secondary is close to filling itsRoche lobe, or it may even be overflowing. The two stars revolve each other along a circular orbit with the components separated by 12.9 times theSun's radius.[3] Due to occultation of each component by the other, the apparent magnitude of the system decreased by 0.3 and 0.4 magnitudes over the course of the binary's orbit, which takes 34 hours 42.6 minutes to complete.
The primary component is aB-typemain sequence star with a stellar classification of B1.5 V. It has 8.3 times themass of the Sun and 3.9 times the Sun's radius. The secondary is a smaller B-type main sequence star with a classification of about B6.5 V, having 3.6 times the Sun's mass and 4.6 times the radius of the Sun. Theeffective temperature of theouter atmosphere for each star is 24,000 K for the primary and 17,000 K for the secondary. At these temperatures, the two stars glow with a blue-white hue.[10]
In 2016, the IAU organized aWorking Group on Star Names (WGSN)[13] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entiremultiple systems.[14] It approved the nameXamidimura for the component Mu1 Scorpii Aa on 5 September 2017 (along withPipirima for the partner of Mu1 Scorpii) and it is now so included in the List of IAU-approved Star Names.[8]
^Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets".arXiv:1012.0707 [astro-ph.SR].
