Simulating the Formation of the Local Group and Other Wide Pairs of Galaxies Within a Cold Dark Matter Cosmogony by Means of a Hierarchical Particle-Mesh Numerical Code

Details Simulating the Formation of the Local Group and Other Wide Pairs of Galaxies Within a Cold Dark Matter Cosmogony by Means of a Hierarchical Particle-Mesh Numerical Code Simulating the Formation of the Local Group and Other Wide Pairs of Galaxies Within a Cold Dark Matter Cosmogony by Means of a Hierarchical Particle-Mesh Numerical Code

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........15g&link_type=abstract

Thesis (PH.D.)--CORNELL UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 56-08, Section: B, page: 4373.

Computer Science

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1

Milky Way-M31 System

Scientific paper

We examine the requisites for a fully self-consistent, collisionless dynamical simulation of the formation of the Local Group of galaxies with sufficient resolution to allow a meaningful test of the tidal torque theory of the origin of galactic angular momentum. Our requirements led us to develop a new, fully adaptive implementation of the Hierarchical Particle-Mesh (HPM) technique, whose performance we test by comparing the results of simulations at both low and high resolution. As initial conditions, we draw pairs of peaks from Gaussian random fields with Cold Dark Matter (CDM) fluctuation spectra normalized to COBE results. We select preferentially wide pairs that are unlikely to coalesce before the present epoch and that have orbital properties comparable to those of the Milky Way-M31 system. Our most detailed runs are capable of achieving 10 kpc resolution within the regions of highest density, which we identify with galactic halos. This is sufficient for the determination of density, velocity dispersion and specific angular momentum profiles within the individual halos. The properties of our simulated halos are roughly compatible with existing observational data for galaxies similar to the Milky Way. It appears that a flat Lambda-CDM model with H_0 = 50 km s^{-1} Mpc ^{-1} and Omega = 0.4 has difficulty producing halos with sufficiently large circular velocities. The angular momenta of successive mass shells within a halo often have very different orientations, making it difficult to predict the orientation of a gaseous disk embedded in the halo. The orbital angular momenta of the pairs are dominated by tidal torques external to the pairs themselves, rather than by the reaction to the spinning up of the halos in each pair.

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