Decaying turbulence in molecular clouds: how does it affect filament networks and star formation?

被引:0
作者
Dhandha, Jiten [1 ,2 ,3 ]
Faes, Zoe [1 ,4 ]
Smith, Rowan J. [1 ,5 ]
机构
[1] Univ Manchester, Jodrell Bank Ctr Astrophys, Dept Phys & Astron, Manchester M13 9PL, England
[2] Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England
[3] Kavli Inst Cosmol, Madingley Rd, Cambridge CB3 0HA, England
[4] ESAC, European Space Agcy, Camino Bajo Castillo S-N,Urb Villafranca del Cast, E-28692 Villanueva De La Canada, Madrid, Spain
[5] Univ St Andrews, SUPA Sch Phys & Astron, St Andrews KY17 9SS, Fife, Scotland
关键词
turbulence; software: public release; stars: formation; ISM: clouds; ISM: structure; INITIAL MASS FUNCTION; MACH NUMBER RELATION; BROWN DWARFS; GRAVITATIONAL COLLAPSE; STELLAR CLUSTERS; FORMATION EFFICIENCY; FORMATION MECHANISMS; RADIATIVE FEEDBACK; FORMING FILAMENTS; GLOBAL EVOLUTION;
D O I
10.1093/mnras/stae862
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The fragmentation of gas to form stars in molecular clouds is intrinsically linked to the turbulence within them. These internal motions are set at the birth of the cloud and may vary with galactic environment and as the cloud evolves. In this paper, we introduce a new suite of 15 high-resolution 3D molecular cloud simulations using the moving mesh code AREPO to investigate the role of different decaying turbulent modes (mixed, compressive, and solenoidal) and virial ratios on the evolution of a 10(4) M-circle dot molecular cloud. We find that diffuse regions maintain a strong relic of the initial turbulent mode, whereas the initial gravitational potential dominates dense regions. Solenoidal seeded models thus give rise to a diffuse cloud with filament-like morphology, and an excess of brown dwarf mass fragments. Compressive seeded models have an early onset of star-formation, centrally condensed morphologies and a higher accretion rate, along with overbound clouds. 3D filaments identified using DISPERSE and analysed through a new PYTHON toolkit we develop and make publicly available with this work called FIESTA, show no clear trend in lengths, masses and densities between initial turbulent modes. Overbound clouds, however, produce more filaments and thus have more mass in filaments. The hubs formed by converging filaments are found to favour star-formation, with surprisingly similar mass distributions independent of the number of filaments connecting the hub.
引用
收藏
页码:4699 / 4718
页数:20
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