Suppression of bar instability by a massive halo

Details Suppression of bar instability by a massive halo Suppression of bar instability by a massive halo

Jan 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976aj.....81...30h&link_type=abstract

Astronomical Journal, vol. 81, Jan. 1976, p. 30-36.

Astronomy and Astrophysics

Astronomy

45

Astronomical Models, Galactic Evolution, Galactic Structure, Halos, Star Distribution, Dynamic Stability, Mass Distribution, Stabilization, Stellar Motions

Scientific paper

Numerical experiments are performed to determine the effect of a spherical uniform-density mass distribution or halo on the evolution of stellar disks. For a halo with radius much smaller than that of the disk, the large-scale bar-forming instability is prevented by a fixed halo (or core) component containing 60% of the total system mass. Similar results are obtained for a halo component corresponding to the Schmidt (1965) model of the Galaxy. For a uniform-density spherical halo with radius equal to that of the stellar disk, a halo component containing only 40% of the total mass is sufficient to stabilize the bar-forming mode. These results indicate that a large halo is more effective in stabilizing against bar formation than a more centrally condensed core-halo.

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