It consists of two massive, blue O-type supergiant stars. The system has an apparent magnitude of 6.06 and is approximately 5,245 light years distant from Earth. Plaskett’s Star (HR 2422) is a spectroscopic binary star system named after the Canadian astronomer John Stanley Plaskett, who discovered that it was a double star in 1922. The star’s estimated age is 2.4 billion years. The star can be seen without binoculars in good viewing conditions. The star is very similar to the Sun with a mass of 1.08 times solar and a radius 1.3 times being 3.47 times more luminous. It has an apparent magnitude of 5.781 and is approximately 97 light years distant. HD 49933 is a yellow-white dwarf belonging to the stellar class F2 V. S Monocerotis is positioned in the Christmas Tree Cluster in NGC 2264, and is surrounded by the nebula Sharpless 273. The system is approximately 1,000 light years distant from Earth. The system has a stellar classification of O7Ve and is variable from magnitude 4.2 to 4.6. S Monocerotis is a massive variable spectroscopic binary and consists of two stars that cannot be resolved, that orbit each other with a period of 25 years. The star appears to be surrounded by a faint reflection nebula in an area spanning over 10 light years. It is about 10,800 times more luminous than the Sun and has a solar mass of 9 times and a radius 37 times. 13 Monocerotis originated from the cluster NGC 2264, which lies 3.5 degrees to the northeast of the star. It has a visual magnitude of 4.47 and is approximately 1,500 light years distant from Earth. Epsilon Monocerotis lies just to the west of the famous Rosette Nebula, one of the best known diffuse nebulae in the sky.ġ3 Monocerotis is a white supergiant star belonging to the stellar class A0Ib. They have luminosities 20 and 2.5 times that of the Sun, radii 2.2 and 1.2 times solar, and masses 1.9 and 1.25 times that of the Sun. The two components are separated by 12.1 arc seconds. The primary component in the system is a white, class A5 sub giant star with an apparent magnitude of 4.44, and the companion is a yellow-white main sequence dwarf of the spectral type F5, with a visual magnitude of 6.72. Ε Monocerotis (Epsilon Monocerotis) is a double star approximately 128 light years from Earth. It is 2,535 times more luminous than the Sun and has a radius 62 times solar. It has a visual magnitude of 4.37 and is approximately 1,852 light years distant from Earth. Ζ Monocerotis (Zeta Monocerotis) is a massive, luminous, yellow supergiant star and belongs to the stellar class G2Ib. It has an apparent magnitude of 4.15 and is about 375 light years distant from the Sun. Δ Monocerotis (Delta Monocerotis) is a white main sequence star with the stellar classification of A2V. The star has an apparent magnitude of 3.98 and is approximately 645 light years distant from us. It is another orange giant, belonging to the stellar class K1.5III. Γ Monocerotis (Gamma Monocerotis) is the third brightest star in the constellation. They all have masses in excess of 6. Beta Monocerotis A is 3,200 times more luminous than the Sun, while components B and C have 1,600 and 1,300 solar luminosities. All three stars in the system are very similar, spectral class B3 with temperatures around 18,500 K. There is also a fourth companion, a 12th magnitude star, visible nearby, but it is a line-of-sight companion and not physically related to the Beta Monocerotis system. All three components: Beta Monocerotis A, B and C are all B-class stars with circumstellar disks orbiting them. It is the brightest visible star in Monoceros. The system has a combined apparent magnitude of 3.74 and is approximately 700 light years distant from Earth. Β Monocerotis (Beta Monocerotis) is a triple star system requiring binoculars to resolve into individual stars. The star has a stellar mass 2.02 and a radius 10.1 times. It has an apparent magnitude of 3.94 and is approximately 144 light years distant from the Sun. It is an orange giant of K0 III classification. Α Monocerotis (Alpha Monocerotis) is the second brightest star in Monoceros.
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