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The Trapezium or Orion Trapezium Cluster, also known by its Bayer designation of Theta 1 Orionis (θ 1 Orionis), is a tight open cluster of stars in the heart of the Orion Nebula, in the constellation of Orion. It was discovered by Galileo Galilei. On 4 February 1617 he sketched three of the stars (A, C and D), but missed the surrounding ...
The star C is the most massive of the four bright stars at the heart of the cluster. It is an O class blue main sequence star with a B-type main sequence companion. Its high luminosity and large distance (about 1,500 light years ) give it an apparent visible magnitude of 5.1.
It is a multiple star system, composed of a large B-type blue giant and a more massive O-type main-sequence star. The Mintaka system constitutes an eclipsing binary variable star, where the eclipse of one star over the other creates a dip in brightness. Mintaka is the westernmost of the three stars of Orion's Belt, as well as the northernmost. [6]
Pi 4 Orionis (π 4 Ori, π 4 Orionis) is a binary star system in the western part of the Orion constellation. It is visible to the naked eye with an apparent visual magnitude of 3.7. [ 2 ] Based upon an annual parallax shift of 3.1 mass , [ 1 ] it is located roughly 1,050 light-years from the Sun .
The three stars of θ 2 Orionis within the Orion Nebula. θ 2 Orionis consists of three stars in a line, each about an arc-minute from the next. In addition to the well-known three stars, the Washington Double Star Catalog confusingly lists a component D which is actually θ 1 Orionis C. [16] There is one other star brighter than 10th magnitude ...
Pi 5 Orionis (π 5 Ori, π 5 Orionis) is a binary star system in the constellation Orion. It has an apparent visual magnitude of 3.69, [2] which is bright enough to be visible to the naked eye on a clear night. Based upon an annual parallax shift of 2.43 mas, [1] it is around 1,300 light-years distant from the Sun.
V380 Orionis is a multiple star system containing at least three stars. A very faint cool star 9" away is also thought to be gravitationally bound, making it a hierarchical quadruple system. Two infrared sources within NGC 1999 have been listed as companions in some catalogues, [ 7 ] but are not thought to be stars. [ 8 ]
The distance to this system, based upon an annual parallax shift of 3.0 mas, [1] is around 1,090 light-years. This is a single-lined [6] spectroscopic binary star system with an orbital period of 3,068 days and an eccentricity of 0.22. [5] It is a member of the young Lambda Orionis cluster [11] and is roughly 7 million years old. [8]
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