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• W2068743889 abstract "In the context of star and planet formation, understanding the formation of disks is of fundamental importance. Previous studies found that the magnetic field has a very strong impact on the collapse of a prestellar cloud, particularly in possibly suppressing the formation of a disk even for relatively modest values of the magnetic intensity. Since observations infer that cores have a substantial level of magnetization, this raises the question of how disks form. However, most studies have been restricted to the case in which the initial angle, $alpha$, between the magnetic field and the rotation axis equals 0$^circ$. We explore and analyse the influence of non aligned configurations on disk formation. We perform 3D ideal MHD, AMR numerical simulations for various values of $mu$, the ratio of the mass-to-flux to the critical mass-to-flux, and various values of $alpha$. We find that disks form more easily as $alpha$ increases from 0 to 90$^circ$. We propose that as the magnetized pseudo-disks become thicker with increasing $alpha$, the magnetic braking efficiency is lowered. We also find that even small values of $alpha$ ($simeq$ 10-20$^circ$) show significant differences with the alligned case. Within the framework of ideal MHD and for our choice of initial conditions, centrifugally supported disks cannot form for values of $mu$ smaller than $simeq$3, if the magnetic field and the rotation axis are perpendicular, and smaller than about $simeq$5-10 when they are perfectly aligned." @default.
• W2068743889 created "2016-06-24" @default.
• W2068743889 creator A5039072357 @default.
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• W2068743889 date "2009-09-24" @default.
• W2068743889 modified "2023-10-13" @default.
• W2068743889 title "Disk formation during collapse of magnetized protostellar cores" @default.
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• W2068743889 doi "https://doi.org/10.1051/0004-6361/200913008" @default.
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