期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 489, 期 2, 页码 1719-1741出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz2215
关键词
MHD; turbulence; protoplanetary discs; stars: formation; ISM: magnetic fields
资金
- European Research Council under the European Community [339248]
- Australian Research Council [FT130100034, DP130102078, andDP180104235]
- BEIS capital funding via STFC capital grants [ST/K000373/1, ST/R002363/1]
- STFC DiRAC Operations grant [ST/R001014/1]
- STFC [ST/R002363/1, ST/R000832/1, ST/M007618/1, ST/R001049/1, ST/K000373/1, ST/T001550/1, ST/T001348/1, ST/T001569/1, ST/R00689X/1, ST/T001372/1, ST/S002529/1, ST/M007065/1, ST/M007006/1, ST/R001006/1, ST/M007073/1, ST/M006948/1, ST/R001014/1] Funding Source: UKRI
We present results from the first radiation non-ideal magnetohydrodynamics (MHD) simulations of low-mass star cluster formation that resolve the fragmentation process down to the opacity limit. We model 50 M-circle dot turbulent clouds initially threaded by a uniform magnetic field with strengths of 3, 5 10, and 20 times the critical mass-to-magnetic flux ratio, and at each strength, we model both an ideal and non-ideal (including Ohmic resistivity, ambipolar diffusion, and the Hall effect) MHD cloud. Turbulence and magnetic fields shape the large-scale structure of the cloud, and similar structures form regardless of whether ideal or non-ideal MHD is employed. At high densities (10(6) less than or similar to n(H) less than or similar to 10(11) cm(-3)), all models have a similar magnetic field strength versus density relation, suggesting that the field strength in dense cores is independent of the large-scale environment. Albeit with limited statistics, we find no evidence for the dependence of the initial mass function on the initial magnetic field strength, however, the star formation rate decreases for models with increasing initial field strengths; the exception is the strongest field case where collapse occurs primarily along field lines. Protostellar discs with radii greater than or similar to 20 au form in all models, suggesting that disc formation is dependent on the gas turbulence rather than on magnetic field strength. We find no evidence for the magnetic braking catastrophe, and find that magnetic fields do not hinder the formation of protostellar discs.
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