Self-gravity, Resonances, and Orbital Diffusion in Stellar Disks - Archive ouverte HAL Access content directly
Journal Articles The Astrophysical Journal Year : 2015

Self-gravity, Resonances, and Orbital Diffusion in Stellar Disks

(1, 2) , , (1, 2)
1
2

Abstract

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 Fokker-Planck equation once the diffusion tensor is known. We 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 disk we are able to reduce the computation of the diffusion tensor to a one-dimensional integral. We implement this formula for a tapered Mestel disk that is exposed to shot noise and find that we are able to explain analytically the principal features of a numerical simulation of such a disk. In particular the formation of narrow ridges of enhanced density in action space is recovered. As the disk's value of Toomre's Q is reduced and the disk becomes more responsive, there is a transition from a regime of heating in the inner regions of the disk through the inner Lindblad resonance to one of radial migration of near-circular orbits via the corotation resonance in the intermediate regions of the disk. The formalism developed here provides the ideal framework in which to study the long-term evolution of all kinds of stellar disks.

Dates and versions

insu-03644938 , version 1 (19-04-2022)

Identifiers

Cite

Jean-Baptiste Fouvry, James Binney, Christophe Pichon. Self-gravity, Resonances, and Orbital Diffusion in Stellar Disks. The Astrophysical Journal, 2015, 806, ⟨10.1088/0004-637X/806/1/117⟩. ⟨insu-03644938⟩
3 View
0 Download

Altmetric

Share

Gmail Facebook Twitter LinkedIn More