This is a plot of the m=2 mode spectrum of the cored exponential disc model, introduced by Jalali & Hunter (2005) in the complex frequency plane as computed with pyStab. The real frequency ωreal equals m times the pattern speed while the imaginary frequncy ωimag quantifies the growth rate. The white dots correspond with eigenmodes. The colored triangles indicate the position of the same modes as calculated with other codes (Omurkanov & Polyachenko 2014)
Below are the density distributions of four prominent two-armed spiral
modes of the cored exponential disc model. Red is positive density;
blue is negative. The full line indicates the location of the
co-rotation radius; the dashed line marks the location of the outer
Lindblad radius. The names of the modes, as given by Jalali
(2007), are indicated in each panel along with the mode's complex
We used pyStab to investigate how a phase-space groove at fixed angular momentum affects the disc's stability properties and showed that, if a groove exists in a responsive part of phase-space, new modes are triggered. These modes can be fast-growing and even dominate the mode spectrum, as can be seen in the figure below. Here, a groove was carved in phase space around an angular momentum of 433 kpc km s-1 causing new modes to arrise, all more rapidly growing than in the ungrooved model.
Thus, we confirm the hypothesis made by previous authors that spiral patterns beget new spiral patterns by carving grooves in phase space at successively larger radii. Because we are using first-order perturbation theory to construct and compare the eigenmode spectra of grooved and ungrooved models, we can rule out two of the possible origins of the wave patterns observed in simulated grooved disc galaxies as suggested by Sellwood & Lin (1989) : these patterns are not intrinsic modes of the original, ungrooved disc and they are not due to non-linear mode coupling. We do confirm the third possibility raised by these authors: they are true eigenmodes, particular to the grooved disc.