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The Origin and Distribution of Angular Momentum in Galaxies

Published online by Cambridge University Press:  26 May 2016

Joel R. Primack
Joel R. Primack*
Affiliation:
Physics Department, University of California, Santa Cruz, CA 95064, U.S.A.

Abstract

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Cold Dark Matter with a large cosmological constant (ACDM) appears to fit large scale structure observations well. of the possible small scale problems, the Central Cusps and Too Many Satellites problems now appear to be at least partly solved, so Angular Momentum has become the most serious remaining CDM problem. There are actually at least two different angular momentum problems: A. Too much transfer of angular momentum to the dark halo to make big disks, and B. Wrong distribution of specific angular momentum to make spiral galaxies, if the baryonic material has the same angular momentum distribution as the dark matter. the angular momentum of dark matter halos, and presumably that of the galaxies they host, appears to arise largely from the orbital angular momentum of the satellites that they accrete. Since the dark and baryonic matter behave very differently in such accretion events, it is possible that the resulting angular momentum distribution of the baryons is different from that of the dark matter, as required to make the sort of galactic disks that are observed. the latest hydrodynamical simulations give some grounds for hope on this score, but much higher resolution simulations are needed.

Type
Part 14: Angular Momentum
Information
Symposium - International Astronomical Union , Volume 220: Dark Matter in Galaxies , 2004 , pp. 467 - 476
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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