Available formats: HTML | PDF | (gzipped) PostScript
uvby- photometry of high-velocity and metal-poor stars
IX. Effects of orbital chaos in the Galactic halo *
W.J. Schuster 1, 2 and
Christine Allen 2
Received 2 April 1996 / Accepted 12 September 1996
Galactic orbits have been integrated using the Galactic potential model of Allen & Santillán (1991) for 280 halo stars identified in the , [Fe/H] diagram. The effects of chaos upon their orbital structure have been investigated.
A "vertical" surface of section is defined, where Z is plotted versus z each time the orbit crosses the cylinder kpc; this surface of section allows a more complete visualization of the Galactic orbits in phase space, a better understanding of the orbital chaos, and a more direct comparison with observations. "Horizontal" surfaces of section and meridional orbits have also been plotted for all of these halo stars, and have been used to classify the Galactic orbits into the categories box, chaotic, and resonant; 44.3% of the halo orbits are found to show some evidence of chaos.
The observed velocities of the halo stars give poor measures of for the box orbits, and especially for the chaotic orbits. Regressions of [Fe/H] against and , for the total sample and for the chaotic and non-chaotic subsets, show little evidence for a metallicity gradient in the Galactic halo.
The surfaces of section for many of the halo stars ( a third) show some evidence of structure within chaos. Part of this structure is due to the "stickiness" that chaotic orbits experience near the outer KAM tori of families of periodic and quasiperiodic orbits. This "stickiness" has been discussed extensively in the literature. The phase-space clumpiness produced by this "stickiness" may help to explain the "moving groups" found in the solar vicinity and the non-Gaussian velocity distributions observed at the Galactic poles. Also, the "confinement" of the chaotic orbits by a 1:1 resonant family of tube orbits, which passes a few kpc above the Sun, may explain part of the halo duality which has been detected in several studies, such as those of Hartwick (1987) and of Kinman et al. (1994).
Histograms of the observed velocity and of the calculated orbital parameter have been plotted for the 280 halo stars. Structure is seen in both histograms, due mainly to the chaotic orbits; the histogram is non-Gaussian with two peaks, and the histogram has three peaks. Remarkably the structure in these two histograms is correlated and can be explained in relation to the details of the surfaces of section and the "confinement" and "stickiness" phenomena of the chaotic orbits.
Key words: chaos stars: kinematics Galaxy: halo Galaxy: kinematics and dynamics Galaxy: structure
Send offprint requests to: W.J. Schuster. P.O. Box 439027, San Diego, CA, 92143-9027, USA
Online publication: July 3, 1998