ARlogo Annu. Rev. Astron. Astrophys. 1992. 30: 51-74
Copyright © 1992 by . All rights reserved

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3.2 Continuum Modes and the Initial-Value Problem

In the limit as the number of rings in the representation of a disk tends to infinity, there will always be long-wavelength modes whose frequencies cluster together to form a continuum. What is the physical significance of these modes? It is natural to expect their wavefunctions zomega (x, y) to be smooth functions of frequency. Now when one disturbs a disk in any way, for example by having a companion galaxy pass close by, the amount of energy fed into each mode is proportional to the square of the overlap integral

Equation 11 (11)

between the mode's wavefunction and the forcing term f(x). If zomega is a continuous function of omega, Iomega will be one too. So any plausible excitation mechanism will excite all modes with frequencies in some interval, and will thus launch a wave-packet. Since the frequencies of these modes differ slightly from one another, their relative phases will evolve in time, and the packet will gradually disperse.

Actually the situation is rather more complex and interesting than this naive analysis suggests. When all is said and done, we are not so much interested in normal modes per se as in their relation to the initial-value problem; galaxies are only tens to hundreds of dynamical times old, so there is no requirement for warps to be immortal, it is sufficient for them to be reasonably enduring. A set of normal modes can be used to solve the general initial-value problem only if it is complete. Van Kampen's (1955) resolution of the problem posed by the normal modes of an electrostic plasma shows that the complete set of modes of a collisionless system involves objects that do not satisfy a dispersion relation, and have distinctly peculiar wavefunctions.

Vlasov's (1945) search for a plasma's normal modes led him to an undefined integral, which he rather arbitrarily interpreted as a Cauchy principal value. Landau (1946) argued that Vlasov should have deflected his integration contour around the integrand's singularity in such a way as to obtain damped modes. Van Kampen (1955) pointed out that Landau's solutions could not be normal modes, since the system is stable and time-reversible, which implies that all modes have real freqencies. In fact, each of Landau's solutions is a superposition of infinitely many true modes, and damps as these drift out of phase.

Van Kampen showed that the true modes have two remarkable features: (a) they have singular wavefunctions, (i.e., ones that involve a delta-function), and (b) they do not satisfy a dispersion relation omega(k). Rather for every pair (omega, k) there is a van Kampen mode. Evidently the limit N -> infty for a collisionless system of N particles has to be treated with some care.

The situation as regards the normal modes of self-gravitating systems is only now emerging from the work of Mathur (1990), Weinberg (1991), Louis (1992), and others. Spatially limited gravitational systems differ from the classical electrostatic plasma in that there is an upper bound on the dynamical time of any of its constituent particles, namely the time to complete a circular orbit around its periphery. If the entire system pulsates with an even longer period than this, no particle will be in resonance with the pulsation, and the latter will not be damped by loss of energy to resonant particles. (The singularity of Vlasov's integrand, and the damping of Landau's solutions arise precisely from the inevitable presence in a plasma of resonant particles.)

Whenever a gravitational system is capable of oscillating with a period longer than that of any particle, (2) the system will have a discrete normal mode. For example, the Hunter & Toomre criterion, integ dR / Sigma (R) < infty, for the existence of a discrete mode, ensures that there is negligible mass in particles with z-frequencies as low as the pattern speed.

As the structure of a stellar system is made more centrally concentrated, the range spanned by its particles' frequencies broadens and the ``gap'' between zero frequency and the lowest particle frequency shrinks. As the upper boundary of the gap moves towards zero it engulphs and destroys successive discrete modes. But Louis (1992) finds that if the boundary has not long swallowed a mode, it is usually possible to detect in n-body simulations an oscillation very much like the swallowed mode. These relic oscillations do not simply decay like Landau's solutions, but fluctuate in amplitude, presumably in step with the transfer of energy from pulsation to resonant particles and back again.

To date this improved understanding of low-frequency oscillations of stellar systems has not been applied to the bending modes of disks. But it does make one wonder whether disks may not have rather long-lived warped configurations which are neither discrete modes nor the exponentially damped waves studied by Landau. Probably more effort should be given to studying the initial-value problem for disks made up of N rings, since this probably behaves less subtly in the limit N -> infty than do the system's normal modes.

2 Strictly, as Louis (1992) points out, the criterion must be formulated in a way which takes into account any selection rule between mode and particle such as may be imposed by considerations of parity.

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