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Emission nebula in the constellation Orion From Wikipedia, the free encyclopedia
The Flame Nebula, designated as NGC 2024 and Sh2-277, is an emission nebula in the constellation Orion. It is about 1350 light-years away.[1] At that distance, the Flame Nebula lies within the Orion B cloud of the larger Orion Molecular Cloud Complex.
| Emission nebula | |
|---|---|
The Flame Nebula (NGC 2024) - based on Chandra X-Ray and Spitzer Infrared images. | |
| Observation data: J2000.0 epoch | |
| Right ascension | 05h 41m 54s |
| Declination | −01° 51′ 0.0″ |
| Distance | 1350[1] ly (415 pc) |
| Apparent magnitude (V) | 10 |
| Apparent dimensions (V) | 30'x30' |
| Constellation | Orion |
| Physical characteristics | |
| Radius | 6 ly |
| Designations | NGC 2024 and Sharpless 277 |
The bright star Alnitak (ζ Ori), the easternmost star in the Belt of Orion, appears very close to the Flame Nebula in the sky. But the star and nebula are not physically associated with one another. The Flame Nebula contains a young cluster of stars which includes at least one hot, luminous O-type star labeled IRS 2b.[2] The dense gas and dust in the foreground of the nebula heavily obscures the star cluster inside the nebula, making studies at infrared wavelengths most useful.
The energetic ultraviolet light emitted by the central O-type star IRS 2b into the Flame Nebula causes the gas to be excited and heated. The glow of the nebula results from the energy input from this central star. Within the nebula and surrounding the central hot star is a cluster of young, lower-mass stars,[3] 86% of which have circumstellar disks.[4] X-ray observations by the Chandra X-ray Observatory[5][6] show several hundred young stars, out of an estimated population of 800 stars.[7] X-ray and infrared images indicate that the young stars are concentrated near the center of the cluster.[8][9]
The Flame Nebula was observed with ALMA and this study found two populations, which are separated by a molecular cloud. The eastern population is 0.2-0.5 Myr old and has a disk fraction of 45±7%. The western population is slightly older at 1 Myr and has a lower disk fraction of 15±4%.[10] This disk fraction is lower than the one observed in the mid-infrared,[4] but the ALMA survey also observed a smaller region.[10] The eastern part contains the O8 star IRS 2b and the western part contains the B0.5V star IRS 1. Hubble observations have shown that the Flame Nebula contains 4 clear proplyds and 4 candidate proplyds. Three of these are in the older western region and are pointing towards IRS 1. The other 5 are in the younger eastern region and are pointing towards IRS 2b.[11]
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