3,125 research outputs found
Singularity Theory for W-Algebra Potentials
The Landau potentials of -algebra models are analyzed with
algebraic-geometric methods. The number of ground states and the number of
independent perturbations of every potential coincide and can be computed. This
number agrees with the structure of ground states obtained in a previous paper,
namely, as the phase structure of the IRF models of Jimbo et al. The
singularities associated to these potentials are identified.Comment: 11 pp., LaTeX file, UVA-93-4
The Fractal Geometry of the Cosmic Web and its Formation
The cosmic web structure is studied with the concepts and methods of fractal
geometry, employing the adhesion model of cosmological dynamics as a basic
reference. The structures of matter clusters and cosmic voids in cosmological
N-body simulations or the Sloan Digital Sky Survey are elucidated by means of
multifractal geometry. A non-lacunar multifractal geometry can encompass three
fundamental descriptions of the cosmic structure, namely, the web structure,
hierarchical clustering, and halo distributions. Furthermore, it explains our
present knowledge of cosmic voids. In this way, a unified theory of the
large-scale structure of the universe seems to emerge. The multifractal
spectrum that we obtain significantly differs from the one of the adhesion
model and conforms better to the laws of gravity. The formation of the cosmic
web is best modeled as a type of turbulent dynamics, generalizing the known
methods of Burgers turbulence.Comment: 35 pages, 8 figures; corrected typos, added references; further
discussion of cosmic voids; accepted by Advances in Astronom
Turbulence models of gravitational clustering
Large-scale structure formation can be modeled as a nonlinear process that
transfers energy from the largest scales to successively smaller scales until
it is dissipated, in analogy with Kolmogorov's cascade model of incompressible
turbulence. However, cosmic turbulence is very compressible, and vorticity
plays a secondary role in it. The simplest model of cosmic turbulence is the
adhesion model, which can be studied perturbatively or adapting to it
Kolmogorov's non-perturbative approach to incompressible turbulence. This
approach leads to observationally testable predictions, e.g., to the power-law
exponent of the matter density two-point correlation function.Comment: 5 pages; contribution to Spanish Relativity Meeting 2011; based on
arXiv:1202.3011, with a brief discussion of relativistic aspect
Stability of Self-Similar Spherical Accretion
Spherical accretion flows are simple enough for analytical study, by solution
of the corresponding fluid dynamic equations. The solutions of stationary
spherical flow are due to Bondi. The questions of the choice of a physical
solution and of stability have been widely discussed. The answer to these
questions is very dependent on the problem of boundary conditions, which vary
according to whether the accretor is a compact object or a black hole. We
introduce a particular, simple form of stationary spherical flow, namely,
self-similar Bondi flow, as a case with physical interest in which analytic
solutions for perturbations can be found. With suitable no
matter-flux-perturbation boundary conditions, we will show that acoustic modes
are stable in time and have no spatial instability at r=0. Furthermore, their
evolution eventually becomes ergodic-like and shows no trace of instability or
of acquiring any remarkable pattern.Comment: Contribution to Spanish Relativity Meeting (ERE) 2005, held in
Oviedo, AIP Conference Proceedings, based on astro-ph/0511624, 4 page
Scaling laws in the stellar mass distribution and the transition to homogeneity
We present a new statistical analysis of the large-scale stellar mass
distribution in the Sloan Digital Sky Survey (data release 7). A set of
volume-limited samples shows that the stellar mass of galaxies is concentrated
in a range of galaxy luminosities that is very different from the range
selected by the usual analysis of galaxy positions. Nevertheless, the two-point
correlation function is a power-law with the usual exponent
--, which varies with luminosity. The mass concentration
property allows us to make a meaningful analysis of the angular distribution of
the full flux-limited sample. With this analysis, after suppressing the shot
noise, we extend further the scaling range and thus obtain and a
clustering length \redc{--Mpc.} Fractional statistical
moments of the coarse-grained stellar mass density exhibit multifractal
scaling. Our results support a multifractal model with a transition to
homogeneity at about Mpc.Comment: 19 pages, 6 figures; new results: shot noise suppression, fractional
moments, analysis of VL samples; to be published in Advances in Astronom
- …