Modified models of radiation pressure instability in application to 10,
  10$^5$, and 10$^7$ $M_{\odot}$ accreting black holes
  Some of the accreting black holes exhibit much stronger variability patterns
than the usual stochastic variations. Radiation pressure instability is one of
the proposed mechanisms which could account for this effect. We aim to model
luminosity changes for objects with black hole mass of 10, 10$^5$, and 10$^7$
solar masses, using the time-dependent evolution of an accretion disk unstable
due to the dominant radiation pressure. We use a 1-dimensional, vertically
integrated time-dependent numerical scheme which models simultaneous evolution
of the disk and corona, coupled by the vertical mass exchange. We also discuss
the possibility of presence of an inner optically thin flow, namely the
Advection-Dominated Accretion Flow (ADAF). We found that the outburst character
strongly depends on the magnetic field and the outer radius of the disk if this
radius is smaller (due to TDE phenomenon) than the size of the instability zone
in a stationary disk with infinite radius. For microquasars, the dependence on
the magnetic field is monotonic, and the period decreases with the field
strength. For larger black hole masses, the dependence is non-monotonic, and
initial rise of the period is later replaced with the relatively rapid decrease
as the magnetic field continues to rise. Still stronger magnetic field
stabilizes the disk. Our computations confirm that the radiation pressure
instability model can account for heartbeat states in microquasars. Rapid
variability detected in IMBH in the form of Quasi-Periodic Ejection can be
consistent with the model but only if combined with TDE phenomenon. Yearly
repeating variability in Changing Look AGN also requires, in our model, small
outer radius either due to the recent TDE or due to the presence of the gap in
the disk related to the presence of a secondary black hole.
