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Colliding filaments in the molecular cloud G34

文献类型：期刊论文

作者Sun, Mingke9,10; Esimbek, Jarken7,8,9,10; Henkel, Christian6,10; Zhou, Jianjun7,8,9,10; Wu, Gang6,9,10; He, Yuxin7,8,9,10; Li, Dalei7,8,9,10; Tang, Xindi7,8,9,10; Komesh, Toktarkhan4,5; Ma, Yingxiu7,8,10
刊名ASTRONOMY & ASTROPHYSICS
出版日期2025-09-19
卷号701页码:A248
关键词ISM: clouds ISM: kinematics and dynamics ISM: molecules ISM: structure planetary nebulae: individual: G34
ISSN号0004-6361
DOI10.1051/0004-6361/202553851
产权排序1
英文摘要The molecular cloud complex G34 is located at a distance of 2.12 +/- 0.38 kpc and contains two giant filaments, F1 and F2. It is considered a good example of colliding filaments. We mapped these two filaments using the (CO)-C-13 and (CO)-C-12 (J = 1-0) lines that were observed with the 13.7 m millimeter-wavelength telescope of the Purple Mountain Observatory. The fraction of high-column density gas N-H2 > 1.0 x 10(22) cm(-2) in F1 and F2 is 4.16% and 8.33%, respectively, which is lower than the typical value of 10% for giant molecular filaments. Moreover, only one of the 13 dense clumps identified in F1 and F2 correlates with the infrared dust cores traced by the NASA Wide-field Infrared Survey Explorer (WISE) 22 mu m emission. This suggests that F1 and F2 may be in early stages of their evolution and might be forming low-mass stars. We also observe large-scale velocity gradients in F1 and F2. Along the spine of F1, the velocity and line mass increase from the ends toward the center, while in F2, they increase from the northwest to the southeast. These parameters are inversely correlated with the gravitational potential, which may indicate a transformation between kinetic energy and gravitational potential energy between F1 and F2. Furthermore, no H II regions correlate with F1 and F2 in the WISE data of galactic H II regions, which indicates that the gas distribution within F1, as well as the V-shaped structure of F1, is unaffected by feedback from H II regions, but is instead caused by gravitational effects. The material in F1 and F2 is not concentrated at the ends of the filaments, but rather in the middle of F1 and at one end of F2 and therefore does not lead to the edge-collapse effect. The collapse and merging timescales thus do not compete. Finally, we calculated the merging time of F1 and F2. When the angle between the line-of-sight velocity and the direction of the relative velocity between F1 and F2 is 45 degrees, the average relative velocity between F1 and F2 is 1.39 km s(-1). The resulting merging timescale is approximately 4.62 +/- 1.12 Myr. This process might be influenced by additional stellar feedback from ongoing star formation within the filaments.
WOS关键词H II REGION ; STAR-FORMING REGIONS ; PHYSICAL-PROPERTIES ; LARGE-SCALE ; TRIGONOMETRIC PARALLAXES ; CLUSTER-FORMATION ; ACCRETION FLOWS ; MAGNETIC-FIELD ; GALACTIC PLANE ; GOULD BELT
资助项目National Key Research and Development Program of Chinahttps://doi.org/10.13039/501100012166[2023YFA1608000] ; National Key Research and Development Program of Chinahttps://doi.org/10.13039/501100012166[2017YFA0402701] ; National Key R&D Program of China[2024TSYCTD0013] ; Tianshan Talent Training Program[2022E0105] ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region[12173075] ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region[11973076] ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region[12103082] ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region[12403033] ; NSFC[2021-XBQNXZ-028] ; NSFC[XBZG-ZDSYS-202212] ; CAS Light of West China Program[2022D04033] ; Xinjiang Key Laboratory of Radio Astrophysics[2022TSYCLJ0005] ; Tianshan Talent Program of Xinjiang Uygur Autonomous Region ; Youth Innovation Promotion Association CAS ; Xinjiang Uyghur Autonomous Region[QYZDJ-SSW-SLH047] ; CAS Key Research Program of Frontier Sciences[2024VMA0002] ; Chinese Academy of Sciences President's International Fellowship Initiative
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001576190400009
出版者EDP SCIENCES S A
资助机构National Key Research and Development Program of Chinahttps://doi.org/10.13039/501100012166 ; National Key R&D Program of China ; Tianshan Talent Training Program ; Regional Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region ; NSFC ; CAS Light of West China Program ; Xinjiang Key Laboratory of Radio Astrophysics ; Tianshan Talent Program of Xinjiang Uygur Autonomous Region ; Youth Innovation Promotion Association CAS ; Xinjiang Uyghur Autonomous Region ; CAS Key Research Program of Frontier Sciences ; Chinese Academy of Sciences President's International Fellowship Initiative
源URL[http://ir.xao.ac.cn/handle/45760611-7/8166]  
专题恒星形成与演化研究团组
通讯作者Sun, Mingke; Esimbek, Jarken; Henkel, Christian
作者单位1.Netherlands Inst Radio Astron, ASTRON, NL-7991 PD Dwingeloo, Netherlands
2.Ural Fed Univ, 19 Mira St, Ekaterinburg 620002, Russia
3.Al Farabi Kazakh Natl Univ, Fac Phys & Technol, Dept Elect & Astrophys, Alma Ata 050040, Kazakhstan
4.Al Farabi Kazakh Natl Univ, Inst Expt & Theoret Phys, Alma Ata 050040, Kazakhstan
5.Nazarbayev Univ, Energet Cosmos Lab, Astana 010000, Kazakhstan
6.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
7.Xinjiang Key Lab Radio Astrophys, Urumqi 830011, Peoples R China
8.State Key Lab Radio Astron & Technol, A20 Datun Rd, Beijing 100101, Peoples R China
9.Univ Chinese Acad Sci, Beijing 100080, Peoples R China
10.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Peoples R China
推荐引用方式
GB/T 7714		 Sun, Mingke,Esimbek, Jarken,Henkel, Christian,et al. Colliding filaments in the molecular cloud G34[J]. ASTRONOMY & ASTROPHYSICS,2025,701:A248.
APA Sun, Mingke.,Esimbek, Jarken.,Henkel, Christian.,Zhou, Jianjun.,Wu, Gang.,...&Sailanbek, Serikbek.(2025).Colliding filaments in the molecular cloud G34.ASTRONOMY & ASTROPHYSICS,701,A248.
MLA Sun, Mingke,et al."Colliding filaments in the molecular cloud G34".ASTRONOMY & ASTROPHYSICS 701(2025):A248.

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