期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 455, 期 4, 页码 3640-3655出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stv2559
关键词
stars: formation; ISM: clouds; ISM: kinematics and dynamics; ISM: structure
资金
- RAS through their Norman Lockyer Fellowship
- Deutsche Forschungsgemeinschaft (DFG) via the Collaborative Research Centre [SFB 881]
- Deutsche Forschungsgemeinschaft (DFG) via the Priority Programme SPP 1573 Physics of the ISM
- European Research Council under the European Community via the ERC [339177]
- STFC [ST/L000768/1]
- DFG [SFB 881, SPP 1573]
- Science and Technology Facilities Council [ST/L000768/1] Funding Source: researchfish
- STFC [ST/L000768/1] Funding Source: UKRI
We show that hydrodynamic turbulent cloud simulations naturally produce large filaments made up of a network of smaller and coherent subfilaments. Such simulations resemble observations of filaments and fibres in nearby molecular clouds. The subfilaments are dynamical features formed at the stagnation points of the turbulent velocity field where shocks dissipate the turbulent energy. They are a ubiquitous feature of the simulated clouds, which appear from the beginning of the simulation and are not formed by gradual fragmentation of larger filaments. Most of the subfilaments are gravitationally subcritical and do not fragment into cores, however, there is also a significant fraction of supercritical subfilaments which break up into star-forming cores. The subfilaments are coherent along their length, and the residual velocities along their spine show that they are subsonically contracting without any ordered rotation on scales of similar to 0.1 pc. Accretion flows along the subfilaments can feed material into star-forming cores embedded within the network. The overall mass in subfilaments and the number of subfilaments increases as the cloud evolves. We propose that the formation of filaments and subfilaments is a natural consequence of the turbulent cascade in the complex multiphase interstellar medium. Subfilaments are formed by the high wavenumber, small-scale modes in the turbulent velocity field. These are then stretched by local shear motions and gathered together by a combination of low wavenumber modes and gravitational contraction on larger scales, and by doing so build up the extended filaments observed in column density maps.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据