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High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22
Yuan, Jinghua1; Li, Jin-Zeng1; Wu, Yuefang2; Ellingsen, Simon P.3; Henkel, Christian4,5; Wang, Ke6; Liu, Tie7,8; Liu, Hong-Li9; Zavagno, Annie10; Ren, Zhiyuan1; Huang, Ya-Fang1
2018
发表期刊ASTROPHYSICAL JOURNAL
卷号852期号:1
摘要How mass is accumulated from cloud-scale down to individual stars is a key open question in understanding highmass star formation. Here, we present the mass accumulation process in a hub-filament cloud G22 that is composed of four supercritical filaments. Velocity gradients detected along three filaments indicate that they are collapsing with a total mass infall rate of about 440M(circle dot) Myr(-1), suggesting the hub mass would be doubled in six free-fall times, adding up to similar to 2 Myr. A fraction of the masses in the central clumps C1 and C2 can be accounted for through large-scale filamentary collapse. Ubiquitous blue profiles in HCO+. (3-2) and (CO)-C-13. (3-2) spectra suggest a clump-scale collapse scenario in the most massive and densest clump C1. The estimated infall velocity and mass infall rate are 0.31 km s(-1) and 7.2 x. 10(-4)M(circle dot) yr(-1), respectively. In clump C1, a hot molecular core (SMA1) is revealed by the Submillimeter Array observations and an outflow-driving high-mass protostar is located at the center of SMA1. The mass of the protostar is estimated to be 11-15M(circle dot) and it is still growing with an accretion rate of 7 x. 10(-5)M(circle dot) yr(-1). The coexistent infall in filaments, clump C1, and the central hot core in G22 suggests that pre-assembled mass reservoirs (i.e., high-mass starless cores) may not be required to form high-mass stars. In the course of high-mass star formation, the central protostar, the core, and the clump can simultaneously grow in mass via core-fed/disk accretion, clump-fed accretion, and filamentary/cloud collapse.
文章类型Article
关键词Ism: Clouds Ism: Individual Objects (G22) Ism: Kinematics And Dynamics Stars: Formation Stars: Massive
WOS标题词Science & Technology ; Physical Sciences
资助者National Natural Science Foundation of China(11503035 ; National Natural Science Foundation of China(11503035 ; International S&T Cooperation Program of China(2010DFA02710) ; International S&T Cooperation Program of China(2010DFA02710) ; EACOA fellowship ; EACOA fellowship ; DFG(1573 ; DFG(1573 ; 11573036 ; 11573036 ; WA3628-1/1) ; WA3628-1/1) ; 11373009 ; 11373009 ; 11433008 ; 11433008 ; 11403040 ; 11403040 ; 11403041) ; 11403041) ; National Natural Science Foundation of China(11503035 ; National Natural Science Foundation of China(11503035 ; International S&T Cooperation Program of China(2010DFA02710) ; International S&T Cooperation Program of China(2010DFA02710) ; EACOA fellowship ; EACOA fellowship ; DFG(1573 ; DFG(1573 ; 11573036 ; 11573036 ; WA3628-1/1) ; WA3628-1/1) ; 11373009 ; 11373009 ; 11433008 ; 11433008 ; 11403040 ; 11403040 ; 11403041) ; 11403041)
DOI10.3847/1538-4357/aa9d40
关键词[WOS]SPECTRAL ENERGY-DISTRIBUTIONS ; YOUNG STELLAR OBJECTS ; FORMING REGION ; MILKY-WAY ; COMPETITIVE ACCRETION ; GALACTIC PLANE ; GLIMPSE SURVEY ; CORES ; OUTFLOW ; SPITZER
收录类别SCI
语种英语
资助者National Natural Science Foundation of China(11503035 ; National Natural Science Foundation of China(11503035 ; International S&T Cooperation Program of China(2010DFA02710) ; International S&T Cooperation Program of China(2010DFA02710) ; EACOA fellowship ; EACOA fellowship ; DFG(1573 ; DFG(1573 ; 11573036 ; 11573036 ; WA3628-1/1) ; WA3628-1/1) ; 11373009 ; 11373009 ; 11433008 ; 11433008 ; 11403040 ; 11403040 ; 11403041) ; 11403041) ; National Natural Science Foundation of China(11503035 ; National Natural Science Foundation of China(11503035 ; International S&T Cooperation Program of China(2010DFA02710) ; International S&T Cooperation Program of China(2010DFA02710) ; EACOA fellowship ; EACOA fellowship ; DFG(1573 ; DFG(1573 ; 11573036 ; 11573036 ; WA3628-1/1) ; WA3628-1/1) ; 11373009 ; 11373009 ; 11433008 ; 11433008 ; 11403040 ; 11403040 ; 11403041) ; 11403041)
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
WOS记录号WOS:000419103300001
引用统计
被引频次:2[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.bao.ac.cn/handle/114a11/20337
专题应用天文研究部
作者单位1.Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China
2.Peking Univ, Dept Astron, Beijing 100871, Peoples R China
3.Univ Tasmania, Sch Phys Sci, Hobart, Tas, Australia
4.Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany
5.King Abdulaziz Univ, Astron Dept, Fac Sci, POB 80203, Jeddah 21589, Saudi Arabia
6.European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany
7.Korea Astron & Space Sci Inst, 776 Daedeokdae Ro, Daejeon 34055, South Korea
8.East Asian Observ, 660 N Aohoku Pl, Hilo, HI 96720 USA
9.Chinese Univ Hong Kong, Dept Phys, Shatin, Hong Kong, Peoples R China
10.Aix Marseille Univ, CNRS, LAM, Marseille, France
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Yuan, Jinghua,Li, Jin-Zeng,Wu, Yuefang,et al. High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22[J]. ASTROPHYSICAL JOURNAL,2018,852(1).
APA Yuan, Jinghua.,Li, Jin-Zeng.,Wu, Yuefang.,Ellingsen, Simon P..,Henkel, Christian.,...&Huang, Ya-Fang.(2018).High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22.ASTROPHYSICAL JOURNAL,852(1).
MLA Yuan, Jinghua,et al."High-mass Star Formation through Filamentary Collapse and Clump-fed Accretion in G22".ASTROPHYSICAL JOURNAL 852.1(2018).
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