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Title:
Contraction of dark matter galactic halos due to baryonic infall
Authors:
Blumenthal, G. R.; Faber, S. M.; Flores, R.; Primack, J. R.
Affiliation:
AA(Lick Observatory, Santa Cruz, CA), AB(Lick Observatory, Santa Cruz, CA), AC(Brandeis University, Waltham, MA), AD(California University, Santa Cruz)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 1, 1986, p. 27-34. (ApJ Homepage)
Publication Date:
02/1986
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
BARYONS, GALACTIC EVOLUTION, GALACTIC ROTATION, GALACTIC STRUCTURE, GRAVITATIONAL COLLAPSE, MISSING MASS (ASTROPHYSICS), ASTRONOMICAL MODELS, HALOS, INTERSTELLAR MATTER, MANY BODY PROBLEM, MASS DISTRIBUTION, SPIRAL GALAXIES
DOI:
10.1086/163867
Bibliographic Code:
1986ApJ...301...27B

Abstract

Varied evidence suggests that galaxies consist of roughly 10 percent baryonic matter by mass and that baryons sink dissipatively by about a factor of 10 in. radius during galaxy formation. It is shown that such infall strongly perturbs the underlying dark matter distribution, pulling it inward and creating cores that are considerably smaller and denser than would have evolved without dissipation. Any discontinuity between the baryonic and dark matter mass distributions is smoothed out by the coupled motions of the two components. If dark halos have large core radii in the absence of dissipation, the above infall scenario yields rotation curves that are flat over large distances, in agreement with observations of spiral galaxies. Such large dissipationless cores may plausibly result from large internal kinetic energy in protogalaxies at maximum expansion, perhaps as a result of subclustering, tidal effects, or anisotropic collapse.

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