2019/12/31 by Rei Enokiya, Akio Ohama, R. Yamada +18 · 36 citations
Chemistry · Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Cloud computing #Collision #Galaxy #Mass distribution #Molecular cloud #Physics #Spectroscopy and Laser Applications #Star (game theory) #Star formation #Stars #Stellar, planetary, and galactic studies #astro-ph.GA
paper · pdf · doi:10.1093/pasj/psaa049
published in Publications of the Astronomical Society of Japan 73(Supplement_1), S256-S272 (Oxford University Press) · 17 pages, 13 figures, accepted for PASJ. arXiv admin note: substantial text overlap with arXiv:1706.05652
arxiv created 2020/05/02 · openalex publication_date 2020/05/06 · arxiv updated 2020/06/24 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract We performed new comprehensive 13CO(J = 2–1) observations toward NGC 2024, the most active star-forming region in Orion B, with an angular resolution of ∼100″ obtained with Nanten2. We found that the associated cloud consists of two independent velocity components. The components are physically connected to the H ii region as evidenced by their close correlation with the dark lanes and the emission nebulosity. The two components show complementary distribution with a displacement of ∼0.6 pc. Such complementary distribution is typical to colliding clouds discovered in regions of high-mass star formation. We hypothesize that a cloud–cloud collision between the two components triggered the formation of the late O-type stars and early B stars localized within 0.3 pc of the cloud peak. The duration time of the collision is estimated to be 0.3 million years from a ratio of the displacement and the relative velocity ∼3 km s−1 corrected for probable projection. The high column density of the colliding cloud ∼1023 cm−2 is similar to those in the other high-mass star clusters in RCW 38, Westerlund 2, NGC 3603, and M 42, which are likely formed under trigger by cloud–cloud collision. The present results provide an additional piece of evidence favorable to high-mass star formation by a major cloud–cloud collision in Orion.