Why haven’t the observed high-frequency QPOs been produced by (MHD) computer simulations of black hole accretion disks?. (arXiv:2112.01415v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Wagoner_R/0/1/0/all/0/1">Robert V. Wagoner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tandon_C/0/1/0/all/0/1">Celia R. Tandon</a> (Dept. of Physics and KIPAC, Stanford University)

We compare some predictions of Wagoner & Tandon (2021) with the results of
the hydrodynamic and magnetohydrodynamic (MHD) simulations of Reynolds & Miller
(2009). It appears that the MHD simulations were not run for long enough and
the numerical damping was not small enough to produce the observed
high-frequency QPOs (and the g-mode seen in the hydro simulations).

We compare some predictions of Wagoner & Tandon (2021) with the results of
the hydrodynamic and magnetohydrodynamic (MHD) simulations of Reynolds & Miller
(2009). It appears that the MHD simulations were not run for long enough and
the numerical damping was not small enough to produce the observed
high-frequency QPOs (and the g-mode seen in the hydro simulations).

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