Massive Neutrino Decay Driven Radiative Instabilities, Sub-Structure Survival in Galaxy Clusters and a Nested - Particle-Mesh Code

Details Massive Neutrino Decay Driven Radiative Instabilities, Sub-Structure Survival in Galaxy Clusters and a Nested - Particle-Mesh Code Massive Neutrino Decay Driven Radiative Instabilities, Sub-Structure Survival in Galaxy Clusters and a Nested - Particle-Mesh Code

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........17s&link_type=abstract

Thesis (PH.D.)--UNIVERSITY OF KANSAS, 1995.Source: Dissertation Abstracts International, Volume: 56-07, Section: B, page: 3807.

Statistics

Methodology

Dark Matter

Scientific paper

I have performed a series of studies concerning the clustering of mass on large scales in the universe, with the goal being an increased understanding of the role of various processes in the formation of structure in the universe. One of the first dark matter candidates was the massive neutrino. In this section I investigate the role of a radiative decay mode for a massive neutrino species, and its impact on structure formation. By reviving a concept known as "mock gravity" I attempt to provide seed masses for eventual galaxy formation in a Hot Dark Matter universe. I show that mock gravity is ineffective at generating seed masses for galaxy formation; the ionization rate is too large and the universe becomes fully ionized well before the radiation pressure can have any effect on the clumping of matter. The final section of this thesis presents a series of N-body experiments which are aimed at understanding the theoretical sources of substructure in galaxy clusters. I perform a series of simulations using a variety of power law initial conditions to generate our cluster data sets. From there I use the statistical methods developed by Bird to analyze the subsequent survival of the sub-structures. I find that for a high omega universe that a significant number of clusters should exhibit sub-structure for very long periods of time after their formation. To test whether the sub-structure results are dependent upon the resolution of the N-body code I develop a nested-grid code for use in performing high resolution studies of gravitational instability. In the next section I present an N-body code which features a nested-grid technology. This nested-grid method allows me to extend both the force and mass resolution of a traditional particle-mesh type code. This code will prove extremely useful for studying problems in large-scale structure formation where one is focusing on highly non -linear objects, and hence force and mass resolution are at a premium. In this chapter I present a review of standard particle-mesh methods, a detailed discussion of my nested -grid methodology along with detailed tests of the algorithm.

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