Institute of Astronomy

Self-Gravity, Resonances & Orbital diffusion in stellar discs

SpeakerTalk DateTalk Series
Jean-Baptiste Fouvry (IAP)30 January 2015Institute of Astronomy Galaxies Discussion Group


Fluctuations in a stellar system’s gravitational field cause the orbits of stars to evolve. The resulting evolution of the system can be computed with the orbit-averaged dressed Fokker-Planck equation in angle-actions coordinates. I will present the formalism that enables one to compute the diffusion tensor from a given source of noise in the gravitational field when the system’s dynamical response to that noise is included. In the case of a cool stellar disc we are able to reduce the computation of the diffusion tensor to a one-dimensional integral. The shot-noise-driven formation of narrow ridges of resonant orbits is therefore recovered in the WKB limit of tightly wound transient spirals, for a tepid Toomre-stable tapered disc, so that we are able to explain analytically the principal features of numerical simulations of such discs.


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