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Table A.3.

List of models calculated for 107 M.

MBH RADAF Rout corona viscosity magnetic magnetic period amplitude amplitude
[M] [Edd] [RSchw] [RSchw] type coefficient disk corona
107 0.20 - 100 - iPtot - - 50.6[y] 104.83 -
107 0.20 - 100 yes iPtot - - 52.6[y] 104.87 102.75
107 0.20 - 50 - iPtot - - 10.1[y] 104.79 -
107 0.20 - 50 yes iPtot - - 12.39[y] 104.97 102.27
107 0.20 - 100 - iPtot Model B 0.01 52.76[y] 104.83 -
107 0.20 - 100 - iPtot Model B 0.05 58.47[y] 104.78 -
107 0.20 - 100 - iPtot Model B 0.1 69.7[y] 104.77 -
107 0.20 - 100 - iPtot Model B 0.2 47.7[y] 104.77 -
107 0.20 - 100 - iPtot Model B 0.4 86.79[y] 104.77 -
107 0.20 - 100 - iPtot Model B 0.5 106.06[y] 104.76 -
107 0.20 - 100 - iPtot Model B 0.7 151.08[y] 104.61 -
107 0.20 - 100 - iPtot Model B 0.8 174.67[y] 104.51 -
107 0.20 - 100 - iPtot Model B 0.9 212.12[y] 104.36 -
107 0.20 - 100 - iPtot Model B 1.0 235.04[y] 104.07 -
107 0.20 - 100 - iPtot Model B 1.1 58.39[y] 102.81 -
107 0.20 - 100 - iPtot Model B 1.15 22.35[y] 102.31 -
107 0.20 - 100 - iPtot Model B 1.25 5.35[y] 100.56 -
107 0.20 - 100 - iPtot Model B 1.5 stable - -
107 0.20 - 100 yes iPtot Model B 0.01 75.33[y] 104.66 102.82
107 0.20 - 100 yes iPtot Model B 0.05 92[y] 104.83 102.81
107 0.20 - 100 yes iPtot Model B 0.1 107.58[y] 104.76 102.65
107 0.20 - 100 yes iPtot Model B 0.2 56.13[y] 104.39 102.88
107 0.20 - 100 yes iPtot Model B 0.4 90.46[y] 104.71 102.83
107 0.20 - 100 yes iPtot Model B 0.5 117.75[y] 104.79 102.53
107 0.20 - 100 yes iPtot Model B 0.7 127.75[y] 104.84 102.01
107 0.20 - 100 yes iPtot Model B 0.8 195.24[y] 104.54 101.93
107 0.20 - 100 yes iPtot Model B 0.9 228.57[y] 104.37 101.83
107 0.20 - 100 yes iPtot Model B 1.0 235.04[y] 104.07 101.59
107 0.20 - 100 yes iPtot Model B 1.1 65.59[y] 102.76 100.48
107 0.20 - 100 yes iPtot Model B 1.15 32.04[y] 102.33 100.18
107 0.20 - 100 yes iPtot Model B 1.2 17.53[y] 101.59 -
107 0.20 - 100 yes iPtot Model B 1.25 stable - -
107 0.20 - 100 yes iPtot Model B 1.5 stable - -

NOTES. Columns are as follows: (1) Black hole mass, (2) accretion rate, (3) the inner ADAF location, (4) the outer radius location, (5) presence of corona, (6) viscosity type, (7) magnetic field model used in the simulation (see Sec. 2.2), (8) magnetic field coefficient used in simulation, (9) period of the outbursts, (10) amplitude of the disk outburst, and (11) amplitude of the corona outburst.

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