Magneto-rotational instability in the protolunar disk
نویسندگان
چکیده
منابع مشابه
Global accretion disk simulations of magneto - rotational instability
We perform global three-dimensional simulations of accretion disks integrating the compressible, non-viscous, but diffusive MHD equations. The disk is supposed to be isothermal. We make use of the ZEUS-3D code integrating the MHD equations and added magnetic diffusivity. We measure the efficiency of the angular-momentum transport. Various model simulations delivered transport parameters of α SS...
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Context. Possible effects of magnetic fields in core collapse supernovae rely on an efficient amplification of the weak pre-collapse fields. It has been suggested that the magneto-rotational instability (MRI) leads to a rapid growth for these weak seed fields. Although plenty of MRI studies exist for accretion disks, the application of their results to core collapse supernovae is inhibited as t...
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Angular momentum transport must have occurred in the Sun’s radiative zone to explain its current solid body rotation. We survey the stability of the early Sun’s radiative zone with respect to diffusive rotational instabilities, for a variety of plausible past configurations. We find that the (faster rotating) early Sun was prone to rotational instabilities even if only weak levels of radial dif...
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How do T Tauri disks accrete? The magneto-rotational instability (MRI) supplies one means, but protoplanetary disk gas is typically too poorly ionized to be magnetically active. Here we show that the MRI can, in fact, explain observed accretion rates for the sub-class of T Tauri disks known as transitional systems. Transitional disks are swept clean of dust inside rim radii of ∼10 AU. Stellar c...
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ژورنال
عنوان ژورنال: Icarus
سال: 2016
ISSN: 0019-1035
DOI: 10.1016/j.icarus.2015.12.042