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Xi Orionis (ξ Orionis) is a binary star system in the northeastern part of the constellation of Orion, well above the red giant star Betelgeuse in the sky. It lies next to another blue main-sequence star, Nu Orionis, which is somewhat closer at 520 light-years' distance.
Meissa / ˈ m aɪ s ə /, designated Lambda Orionis (λ Orionis, abbreviated Lambda Ori, λ Ori) is a star in the constellation of Orion. It is a multiple star approximately 1,300 ly away with a combined apparent magnitude of 3.33. [12] The main components are an O8 giant star and a B-class main sequence star, separated by about 4
V883 Orionis is a protostar in the constellation of Orion. It is associated with IC 430 (Haro 13A), a peculiar Hα object surveyed by Guillermo Haro in 1952. [4] It is assumed to be a member of the Orion Nebula cluster at 414 ± 7 pc. [2] V883 Orionis, like most protostars, is surrounded by a circumstellar disc of dust.
W Orionis is a carbon star in the constellation Orion, approximately 400 parsecs (1,300 ly) away. It varies regularly in brightness between extremes of magnitude 4.4 and 6.9 roughly every 7 months. When it is near its maximum brightness, it is faintly visible to the naked eye of an observer with good observing conditions.
Iota Orionis (ι Orionis, abbreviated ι Ori) is a multiple star system in the equatorial constellation of Orion the hunter. It is the eighth-brightest member of Orion with an apparent visual magnitude of 2.77 and also the brightest member of the asterism known as Orion's Sword. It is a member of the NGC 1980 open cluster.
Rho Orionis, Latinised from ρ Orionis, is the Bayer designation for an orange-hued binary star system in the equatorial constellation of Orion.It is visible to the naked eye with an apparent visual magnitude of +4.44. [2]
GW Orionis is a variable star with quasi-periodic brightness changes. The apparent magnitude varies between 9.7 and 10.4 with dimming events of between 0.1 and 0.7 magnitudes roughly every 30 days, as well as more sinusoidal variations with an amplitude of 0.2 magnitudes over 11.6 years.
This is an A-type main-sequence star with a stellar classification of A3 Va. [3] It is a Lambda Boötis star, [8] which means the spectrum shows lower-than-expected abundances for heavier elements. [9] Pi 1 Orionis is a relatively young star, just 100 million years old, [5] and is spinning fairly rapidly with a projected rotational velocity of ...