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![Absolute optical magnitudes of IPs versus their P orb. Outbursts and low states are marked by the empty circles and squares, respectively (most data are from [30] and [31]). GK Per lies out of range. The relation between P orb and the peak brightness of outbursts of dwarf novae and their quiescent level are according to [30]. The plot is updated from [23].](publication/323920899/figure/fig4/AS:606783966023689@1521679979876/Absolute-optical-magnitudes-of-IPs-versus-their-P-orb-Outbursts-and-low-states-are.png)
Absolute optical magnitudes of IPs versus their P orb. Outbursts and low states are marked by the empty circles and squares, respectively (most data are from [30] and [31]). GK Per lies out of range. The relation between P orb and the peak brightness of outbursts of dwarf novae and their quiescent level are according to [30]. The plot is updated from [23].
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Context 1
... optical magnitudes in Fig. 4 show that most IPs lie between those of dwarf novae (DNe) in outburst and quiescence. This enables to assess the conditions in V1223 Sgr in the context of the long-term activity of the IPs. Fig. 4 shows that a thermal-viscous instability of the accretion disk [22] should be present in most IPs. This should lead to DN outbursts modified by a truncation of the inner disk region by the magnetic field of the WD. The model of [1] predicts that these outbursts will be shorter if the inner disk region is truncated by the magnetic field of the WD and if the heating front which switches the disk from the cool to the hot state (outburst) starts in the outer disk region and propagates toward the WD (so if the outburst is of the outside-in type). [30] and [31]). GK Per lies out of range. The relation between P orb and the peak brightness of outbursts of dwarf novae and their quiescent level are according to [30]. The plot is updated from ...
Context 2
... optical magnitudes in Fig. 4 show that most IPs lie between those of dwarf novae (DNe) in outburst and quiescence. This enables to assess the conditions in V1223 Sgr in the context of the long-term activity of the IPs. Fig. 4 shows that a thermal-viscous instability of the accretion disk [22] should be present in most IPs. This should lead to DN outbursts modified by a truncation of the inner disk region by the magnetic field of the WD. The model of [1] predicts that these outbursts will be shorter if the inner disk region is truncated by the magnetic field of the WD and if the heating front which switches the disk from the cool to the hot state (outburst) starts in the outer disk region and propagates toward the WD (so if the outburst is of the outside-in type). [30] and [31]). GK Per lies out of range. The relation between P orb and the peak brightness of outbursts of dwarf novae and their quiescent level are according to [30]. The plot is updated from ...
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