Gould Belt
The Gould Belt is a partial ring of stars local to us in the Milky Way. It is about 3000 light years across, tilted from the galactic plane by 16 to 20 degrees. It has many large and bright O- and B-type stars.[1]
The belt may be the local spiral arm to which the Sun belongs. At present the Sun is about 325 light years from the arm's centre. The belt is thought to be from 30 to 50 million years old, and of unknown origin. Benjamin Gould identified it in 1879.[2][3][4]
The belt contains bright stars in many constellations including (in order going more or less eastward) Cepheus, Lacerta, Perseus, Orion, Canis Major, Puppis, Vela, Carina, Crux (the Southern Cross), Centaurus, Lupus, and Scorpius (including the Scorpius-Centaurus Association).
Overview
changeStar-forming regions with bright O and B stars make up the Gould Belt. These regions include the Orion Nebula and the Orion molecular clouds, the Scorpius-Centaurus OB Association, Cepheus OB2, Perseus OB2, and the Taurus-Auriga Molecular Clouds.
A theory proposed around 2009 suggests that the Gould Belt formed about 30 million years ago when a blob of dark matter collided with the molecular cloud in our region. There is also evidence for similar Gould belts in other galaxies.[5][6]
Related pages
change- Radcliffe wave, a recent description of our local area of the galaxy.
References
change- ↑ Alves, João and others 2020. A galactic-scale gas wave in the solar neighbourhood. Nature Accelerated Article Preview. [1]
- ↑ Patrick Moore, ed. (2002) [1987]. Astronomy Encyclopædia (Revised ed.). Great Britain: Philip's. p. 164. ISBN 9780540078639.
- ↑ "The Gould Belt". The GAIA Study Report. Retrieved 2006-07-18.
- ↑ "Gould Belt". The Encyclopedia of Astrobiology, Astronomy and Spaceflight. Retrieved 2006-07-18.
- ↑ "Orion's dark secret: Violence shaped the night sky", New Scientist, 21 Nov. 2009, pp. 42–5.
- ↑ Bekki, Kenji (2009). "Dark impact and galactic star formation: origin of the Gould belt". Monthly Notices of the Royal Astronomical Society: Letters. 398 (1): L36–L40. arXiv:0906.5117. Bibcode:2009MNRAS.398L..36B. doi:10.1111/j.1745-3933.2009.00702.x. S2CID 16173683. Archived from the original on 2012-12-08.
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