The competition between the hydrodynamic instability from noise and magnetorotational instability in the Keplerian disks

We venture for the comparison between growth rates for magnetorotational instability (MRI) and hydrodynamics instability in the presence of an extra force in the local Keplerian accretion flow. The underlying model is described by the Orr–Sommerfeld and Squire equations in the presence of rotation, magnetic field, and an extra force, plausibly noise with a nonzero mean. We obtain MRI using the Wentzel–Kramers–Brillouin approximation without extra force for a purely vertical magnetic field and vertical wavevector of the perturbations. Expectedly, MRI is active within a range of magnetic field, which changes depending on the perturbation wavevector magnitude. Next, to check the effect of noise on the growth rates, a quartic dispersion relation has been obtained. Among those four solutions for the growth rate, the one that reduces to the MRI growth rate at the limit of vanishing mean of noise in the MRI active region of the magnetic field is mostly dominated by MRI. However, in the MRI inactive region, in the presence of noise, the solution turns out to be unstable, which is almost independent of the magnetic field. Another growth rate, which is almost complementary to the previous one, leads to stability at the limit of vanishing noise. The remaining two growth rates, which correspond to the hydrodynamical growth rates at the limit of the vanishing magnetic field, are completely different from the MRI growth rate. More interestingly, the latter growth rates are larger than that of the MRI. If we consider viscosity, the growth rates decrease depending on the Reynolds number.