High-mass star formation in the Large Magellanic Cloud triggered by colliding H <scp>i</scp> flows-Reference-Cited by-同舟云学术

High-mass star formation in the Large Magellanic Cloud triggered by colliding H i flows

Published:2024-05-24 Issue:4 Volume:76 Page:589-615
ISSN:0004-6264
Container-title:Publications of the Astronomical Society of Japan
language:en
Short-container-title:

Author:

Tsuge Kisetsu¹²³⁴^ORCID,Sano Hidetoshi³^ORCID,Tachihara Kengo⁵^ORCID,Bekki Kenji⁶,Tokuda Kazuki⁷⁸^ORCID,Inoue Tsuyoshi⁹,Mizuno Norikazu⁷,Kawamura Akiko⁷,Onishi Toshikazu¹⁰,Fukui Yasuo⁵

Affiliation:

1. Department of Physics, Graduate School of Science, University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan

2. Institute for Advanced Study, Gifu University , 1-1 Yanagido, Gifu, Gifu 501-1193, Japan

3. Faculty of Engineering, Gifu University , 1-1 Yanagido, Gifu, Gifu 501-1193, Japan

4. Institute for Advanced Research, Nagoya University , Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan

5. Department of Physics, Nagoya University , Furo-cho, Chikusa-ku, Nagoya, Aichi 464-8601, Japan

6. ICRAR, M468, University of Western Australia , 35 Stirling Highway, Crawley, Perth WA 6009, Australia

7. National Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan

8. Department of Earth and Planetary Sciences, Faculty of Science, Kyushu University , Nishi-ku, Fukuoka, Fukuoka 819-0395, Japan

9. Department of Physics, Faculty of Science and Engineering, Konan University , 8-9-1 Okamoto, Higashinada-ku, Kobe, Hyogo 658-8501, Japan

10. Department of Physics, Graduate School of Science, Osaka Metropolitan University , 1-1 Gakuen-cho, Naka-ku, Sakai, Osaka 599-8531, Japan

Abstract

Abstract The galactic tidal interaction is a possible mechanism to trigger active star formation in galaxies. Recent analyses using H i data in the Large Magellanic Cloud (LMC) proposed that the tidally driven H i flow, the L-component, is colliding with the LMC disk, the D-component, and is triggering high-mass star formation toward the active star-forming regions R136 and N44. In order to explore the role of the collision over the entire LMC disk, we investigated the I-component, the collision-compressed gas between the L- and D-components, over the LMC disk, and found that $74\%$ of the O/WR stars are located toward the I-component, suggesting their formation in the colliding gas. We compared four star-forming regions (R136, N44, N11, and the N77–N79–N83 complex). We found a positive correlation between the number of high-mass stars and the compressed gas pressure generated by collisions, suggesting that pressure may be a key parameter in star formation.

Funder

Japan Society for the Promotion of Science

Australian Research Council

National Aeronautics and Space Administration

University of Michigan

Publisher

Oxford University Press (OUP)

Link

https://academic.oup.com/pasj/article-pdf/76/4/589/58712783/psae035.pdf

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