25 Orionis

25 Orionis, less commonly known by its Bayer designation Psi1 Orionis (ψ1 Orionis, ψ1 Ori) is a fifth-magnitude star in the constellation Orion. It lies among a dense cluster of low-mass pre-main-sequence stars in the Orion OB1a. 25 Orionis is the dominant member of a rich low-mass star region, first identified in 2005 in a statistical analysis of 2.5 million stars. It is one of several sub-associations within Orion OB1a, all thought to lie at around the same distance of 338 parsecs. Over 200 members of the 25 Orionis stellar group have been found, mostly T Tauri stars with spectral types of K and M and masses less than half the sun's. There are also around 60 hotter stars in the region, including the eruptive variable V346 Tauri. This region is known as Briceño 1. Like the star Pleione in the Pleiades open cluster, 25 Ori is a Be star with a gaseous circumstellar disk. The SIMBAD astronomical database lists its spectral class as B1Vn. 25 Orionis is a fast rotator, clocking a rotational velocity of 316 km/s, significantly faster than Achernar's speed of 251 km/s in the constellation Eridanus. Having a radius of , the star rotates on its axis roughly once every 23 hours. With a mass in excess of , the star is expected to explode as a supernova. 25 Orionis is a Gamma Cassiopeiae variable star, and has been given the variable star designation V1086 Orionis. The General Catalog of Variable Stars lists its magnitude as varying between magnitude 4.92 and 4.96 in the visual (V) band - an amplitude only 0.04 magnitudes. However photometry by the Hipparcos satellite, which had a passband broader than the V band, showed a 0.145 magnitude range in brightness.