Draft:Monoceros R1
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| Molecular cloud | |
|---|---|
 Image of Monoceros R1. | |
| Observation data: J2000 epoch | |
| Right ascension | 06h 31m 60s[1] |
| Declination | +10° 11′ 60″[1] |
| Distance | ~2,300[2] ly |
| Constellation | Monoceros |
| Designations | Monoceros R1 Ring, Monoceros R1 Association[1] |
Monoceros R1 Molecular Cloud Complex, also known as the Monoceros R1 Ring is a young stellar association and predominantly unilluminated molecular cloud complex located roughly 2,300 light-years (ly) away in the constellation Monoceros on the galactic plane. Monoceros R1, along with the Monoceros OB1 association forms a minor part of the larger Monoceros OB1 Molecular Cloud.[2]
Observations
[edit]
The complex contains a large number of reflection nebulae illuminated by the Monoceros R1 OB association, this stellar association formed at the same time as the Monoceros OB1 association, these associations were formed by turbulent winds from the main Monoceros OB1 Molecular Cloud. The stars of Monoceros R1 are mostly T Tauri emission line stars or B-type stars.[3] Most of the B-type stars are located in Collinder 95, an open cluster that created reflection nebula IC 447 via supernovae.[2][4]
Unlike the rest of the Monoceros OB1, Monoceros R1 does not produce high-mass stars, most of the stars produced are usually intermediate or low-mass stars. The region also has a halo of escaping stars.[5]
Structure
[edit]Monoceros R1 is located near Sh 2-273 and is adjacent to the massive H II region NGC 2264. Monoceros R1 exhibits a ring like structure composed of dust clouds and reflection nebulae. This ring appears to be kinematically different from the rest of the Monoceros OB1 Molecular Cloud, this ring and its components seem to located further away than the components of NGC 2264. NGC 2264 primarily contains high-velocity materials while lower-velocity materials is located near or in Monoceros R1. The reflection nebulae IC 447, IC 446, VdB 76, VdB 77, NGC 2247, and NGC 2245 are members of Monoceros R1, this is because they are kinematically different. Portions of the molecular clouds in the north like Barnard 37 are likely not members of Monoceros R1. Dark nebula LDN 1607 connects IC 446 to IC 447.[6][7]
The ring has a diameter of approximately 12 pc and an average thickness of 2 pc. The carbon dioxide (CO) emissions in VdB 77, VdB 82, and NGC 2245 suggest that Monoceros R1 experienced shock-induced heating. The ring of Monoceros R1 most likely formed roughly one million years ago by a supernova blast wave, stellar wind, or an expending H II region.[6] A massive filament between IC 446 and IC 447 with a length of around 14 pc formed these reflection nebulae. Thid filament contains an estimated mass of approximately 7,000 M☉.[8][9]
References
[edit]- 1 2 3 "NAME Mon R1". simbad.cds.unistra.fr.
- 1 2 3 Lim, Beomdu; Nazé, Yaël; Hong, Jongsuk; Yoon, Sung-yong; Lee, Jinhee; Hwang, Narae; Park, Byeong-Gon; Lee, Jeong-Eun (June 2022). "A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations". The Astronomical Journal. 163 (6): 266. arXiv:2204.00444. Bibcode:2022AJ....163..266L. doi:10.3847/1538-3881/ac63b6.
- ↑ Ogura, K. (March 1984). "New Hα-Emission Stars in Monoceros OB1 and R1 Associations". Publications of the Royal Astronomical Society of Japan. 36 (1): 139–148. Bibcode:1984PASJ...36..139O. doi:10.1093/pasj/36.1.139.
- ↑ Magakian, T. Yu.; Tatarnikov, A. M.; Movsessian, T. A.; Adreasyan, H. R. (February 2022). "Near-infrared detection of H2 flows in the core of the Mon R1 association". Monthly Notices of the Royal Astronomical Society. 510 (2): 2139–2146. arXiv:2112.05196. Bibcode:2022MNRAS.510.2139M. doi:10.1093/mnras/stab3585.
- ↑ Movsessin, T. A.; Magakian, T. Yu.; Dodonov, S. N. (November 2020). "New Herbig-Haro objects and outflows in Mon R1 association". Monthly Notices of the Royal Astronomical Society. 500 (2): 2440–2450. arXiv:2005.04257. doi:10.1093/mnras/staa3302.
- 1 2 Kutner, M. L.; Dickman, R. L.; Tucker, K. D.; Machnik, D. E. (September 1979). "Ring structure in the Monoceros R1 molecular clouds". Astrophysical Journal. 232 (1): 724–728. Bibcode:1979ApJ...232..724K. doi:10.1086/157332.
- ↑ Cambrésy, L. (May 1999). "Mapping of the extinction in giant molecular clouds using optical star counts". Astronomy and Astrophysics. 345: 965–976. arXiv:astro-ph/9903149. Bibcode:1999A&A...345..965C.
- ↑ Bhadari, N. K.; Dewangan, L. K.; Pirogov, L. E.; Ojha, D. K. (August 2020). "Star-forming Sites IC 446 and IC 447: An Outcome of End-dominated Collapse of Monoceros R1 Filament". The Astrophysical Journal. 899 (2): 167. arXiv:2006.13894. Bibcode:2020ApJ...899..167B. doi:10.3847/1538-4357/aba2c6.
- ↑ Machnik, D. E. (1981). "Observations of Molecular Clouds Containing Reflection Nebulae". Dissertation Abstracts International. 42–04: 1495. Bibcode:1981PhDT.........3M.