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- W2563517752 abstract "We investigate the role of magnetic fields in the fragmentation of self-gravitating discs using 3D global ideal magnetohydrodynamic simulations performed with the phantom smoothed particle hydrodynamics code. For initially toroidal fields, we find two regimes. In the first, where the cooling time is greater than five times the dynamical time, magnetic fields reduce spiral density wave amplitudes, which in turn suppresses fragmentation. This is the case even if the magnetic pressure is only a tenth of the thermal pressure. The second regime occurs when the cooling time is sufficiently short that magnetic fields cannot halt fragmentation. We find that magnetised discs produce more massive fragments, due to both the additional pressure exerted by the magnetic field, and the additional angular momentum transport induced by Maxwell stresses. The fragments are confined to a narrower range of initial semimajor axes than those in unmagnetised discs. The orbital eccentricity and inclination distributions of unmagnetised and magnetised disc fragments are similar. Our results suggest the fragmentation boundary could be at cooling times a factor of two lower than predicted by purely hydrodynamical models." @default.
- W2563517752 created "2017-01-06" @default.
- W2563517752 creator A5013805663 @default.
- W2563517752 creator A5018695775 @default.
- W2563517752 creator A5023421226 @default.
- W2563517752 date "2016-12-20" @default.
- W2563517752 modified "2023-10-18" @default.
- W2563517752 title "On the fragmentation boundary in magnetized self-gravitating discs" @default.
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- W2563517752 doi "https://doi.org/10.1093/mnras/stw3314" @default.
- W2563517752 hasPublicationYear "2016" @default.
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