Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.106..309c&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 106, no. 2, Nov. 1984, p. 309-339.
Astronomy and Astrophysics
Astrophysics
18
Galactic Evolution, Galactic Structure, Ring Galaxies, Astronomical Models, Collisions, Disk Galaxies, Mass Distribution, Stellar Motions
Scientific paper
The conditions under which a head-on collision between a disk galaxy and a spherical galaxy can lead to ring formation are investigated, using the impulsive approximation. The spherical galaxy is modeled as a polytrope of index n = 4 and radius RS and the disk galaxy as an exponential disk. Calculations are made for the case RS = RD. Since practically the entire mass of the spherical galaxy, for the chosen model, lies within 1/3 of its radius, the radius of the spherical galaxy is effectively 1/3 that of the disk galaxy. It is found that as a result of the collision, the innermost and the outer parts of the disk galaxy are not much affected, but the intermediate region expands and gets evacuated, leading to the crowding of stars in a preferential region forming a ring structure. The rings are best formed for a normal, on-axis collision.
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