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- W2332949658 abstract "The magnetorotational instability (MRI) is a shear instability and thus its sensitivity to the shear parameter $q = - dlnOmega/dln r $ is of interest to investigate. Motivated by astrophysical disks, most (but not all) previous MRI studies have focused on the Keplerian value of $ q=1.5$. Using simulation with 8 vertical density scale heights, we contribute to the subset of studies addressing the the effect of varying $q$ in stratified numerical simulations. We discuss why shearing boxes cannot easily be used to study $q>2$ and thus focus on $q<2$. As per previous simulations, which were either unstratified or stratified with a smaller vertical domain, we find that the $q$ dependence of stress for the stratified case is not linear, contrary to the Shakura-Sunyaev model. We find that the scaling agrees with cite{1996MNRAS.281L..21A} who found it to be proportional to the shear to vorticity ratio $q/(2-q)$. We also find however, that the shape of the magnetic and kinetic energy spectra are relatively insensitive to $q$ and that the ratio of Maxwell stress to magnetic energy ratio also remains nearly independent of $q$. This is consistent with a theoretical argument in which the rate of amplification of the azimuthal field depends linearly on $q$ and the turbulent correlation time $tau$ depends inversely on $q$. As such, we measure the correlation time of the turbulence and find that indeed it is inversely proportional to $q$." @default.
- W2332949658 created "2016-06-24" @default.
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- W2332949658 date "2016-01-27" @default.
- W2332949658 modified "2023-10-16" @default.
- W2332949658 title "Erratum: sensitivity of the magnetorotational instability to the shear parameter in stratified simulations" @default.
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- W2332949658 doi "https://doi.org/10.1093/mnras/stw032" @default.
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