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Title:
Resonant excitation of motion perpendicular to galactic planes
Authors:
Binney, J.
Affiliation:
AA(Princeton University, New Observatory, Princeton, NJ)
Publication:
Royal Astronomical Society, Monthly Notices, vol. 196, Aug. 1981, p. 455-467. (MNRAS Homepage)
Publication Date:
08/1981
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
DISK GALAXIES, ELLIPTICAL GALAXIES, GALACTIC NUCLEI, STELLAR MOTIONS, ECCENTRIC ORBITS, EQUATIONS OF MOTION, MOTION STABILITY, STELLAR OSCILLATIONS
Comment:
A&AA ID. AAA030.151.002
Bibliographic Code:
1981MNRAS.196..455B

Abstract

Resonant coupling between oscillations perpendicular to the equatorial plane of a galaxy and periodic changes in the force towards the Galactic Center can cause stars to move far from the plane. The variation of the force to the Galactic Center may be caused by a non-axisymmetric potential, but instability is possible even in the axisymmetric case. The circumstances under which these instabilities occur in highly flattened potentials and in nearly spherical systems are discussed. This work clarifies the restrictions that may be placed on the shapes of elliptical galaxies from observations of their nuclear disks. However, it appears that the most important instability is one experienced by stars that orbit at large radii in the disk of a galaxy which has a rotating central bar. Any barred galaxy will have an annulus of such stars. The mechanism discussed here may help in the understanding of (1) warps and corrugations in the gaseous discs of galaxies, (2) the kinematics of stars in the solar neighborhood, and (3) the sharp edges possessed by many stellar disks.

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