Lambda Orionis Cluster

southern hemisphere

ellipticity of 0.06, carrying it as far as 28 kly (8.6 kpc) from the Galactic Center, and as close as 25 kly (7.7 kpc). The inclination of the orbit carries it up to 260 light-years (80 parsecs) away from the galactic plane. On average it crosses the plane every 33.3 million years.^[1]

low-mass stars, some T Tauri stars and brown dwarfs.^[3][4] One notable member is LOri167, which is a wide binary consisting of a potential planetary-mass object and a brown dwarf.^[5] Observations of the star cluster with the Spitzer Space Telescope have shown that 25% of the low-mass stars and 40% of the substellar objects are surrounded by a circumstellar disk.^[4] Two of these being actively photoevaporated by Meissa.^[6]

low-mass stars formed in the central regions of these clouds. The low-mass stars closest to the massive stars likely lost their circumstellar disks due to photoevaporation. Many low-mass stars parsecs away were unaffected by this and represent the current population of low-mass stars with a circumstellar disk. The cluster is surrounded by a large molecular ring, called the Lambda Orionis ring. This was interpreted as a remnant of a supernova that exploded one million years ago. The supernova blast encountered the clouds and gas in the region and the blast dispersed the parent core, creating the molecular ring.^[7]