11,700 research outputs found
Galaxy Formation Spanning Cosmic History
Over the past several decades, galaxy formation theory has met with
significant successes. In order to test current theories thoroughly we require
predictions for as yet unprobed regimes. To this end, we describe a new
implementation of the Galform semi-analytic model of galaxy formation. Our
motivation is the success of the model described by Bower et al. in explaining
many aspects of galaxy formation. Despite this success, the Bower et al. model
fails to match some observational constraints and certain aspects of its
physical implementation are not as realistic as we would like. The model
described in this work includes substantially updated physics, taking into
account developments in our understanding over the past decade, and removes
certain limiting assumptions made by this (and most other) semi-analytic
models. This allows it to be exploited reliably in high-redshift and low mass
regimes. Furthermore, we have performed an exhaustive search of model parameter
space to find a particular set of model parameters which produce results in
good agreement with a wide range of observational data (luminosity functions,
galaxy sizes and dynamics, clustering, colours, metal content) over a wide
range of redshifts. This model represents a solid basis on which to perform
calculations of galaxy formation in as yet unprobed regimes.Comment: MNRAS accepted. Extended version (with additional figures and details
of implementation) is available at http://www.galform.or
A locally adaptive time-stepping algorithm for\ud petroleum reservoir simulations
An algorithm for locally adapting the step-size for large scale finite volume simulations of multi-phase flow in petroleum reservoirs is suggested which allows for an “all-in-one” implicit calculation of behaviour over a very large time scale. Some numerical results for simple two-phase flow in one space dimension illustrate the promise of the algorithm, which has also been applied to very simple 3D cases. A description of the algorithm is presented here along with early results. Further development of the technique is hoped to facilitate useful scaling properties
Numerical solution of a non-linear conservation law applicable to the interior dynamics of partially molten planets
The energy balance of a partially molten rocky planet can be expressed as a
non-linear diffusion equation using mixing length theory to quantify heat
transport by both convection and mixing of the melt and solid phases. In this
formulation the effective or eddy diffusivity depends on the entropy gradient,
, as well as entropy. First we present a simplified
model with semi-analytical solutions, highlighting the large dynamic range of
, around 12 orders of magnitude, for physically-relevant
parameters. It also elucidates the thermal structure of a magma ocean during
the earliest stage of crystal formation. This motivates the development of a
simple, stable numerical scheme able to capture the large dynamic range of
and provide a flexible and robust method for
time-integrating the energy equation.
We then consider a full model including energy fluxes associated with
convection, mixing, gravitational separation, and conduction that all depend on
the thermophysical properties of the melt and solid phases. This model is
discretised and evolved by applying the finite volume method (FVM), allowing
for extended precision calculations and using as the
solution variable. The FVM is well-suited to this problem since it is naturally
energy conserving, flexible, and intuitive to incorporate arbitrary non-linear
fluxes that rely on lookup data. Special attention is given to the numerically
challenging scenario in which crystals first form in the centre of a magma
ocean.
Our computational framework is immediately applicable to modelling high melt
fraction phenomena in Earth and planetary science research. Furthermore, it
provides a template for solving similar non-linear diffusion equations arising
in other disciplines, particularly for non-linear functional forms of the
diffusion coefficient
Massive and Red Objects predicted by a semianalytical model of galaxy formation
We study whether hierarchical galaxy formation in a concordance CDM
universe can produce enough massive and red galaxies compared to the
observations. We implement a semi-analytical model in which the central black
holes gain their mass during major mergers of galaxies and the energy feedback
from active galaxy nuclei (AGN) suppresses the gas cooling in their host halos.
The energy feedback from AGN acts effectively only in massive galaxies when
supermassive black holes have been formed in the central bulges. Compared with
previous models without black hole formation, our model predicts more massive
and luminous galaxies at high redshift, agreeing with the observations of K20
up to . Also the predicted stellar mass density from massive galaxies
agrees with the observations of GDDS. Because of the energy feedback from AGN,
the formation of new stars is stopped in massive galaxies with the termination
of gas cooling and these galaxies soon become red with color 5 (Vega
magnitude), comparable to the Extremely Red Objects (EROs) observed at redshift
1-2. Still the predicted number density of very EROs is lower than
observed at , and it may be related to inadequate descriptions of dust
extinction, star formation history and AGN feedback in those luminous galaxies.Comment: Accepted for Publication in ApJ, added reference
Study of thin film large area photovoltaic solar energy converter Final report
Thin film large area cadmium sulfide solar cell
Study of thin film large area photovoltaic solar energy converter Third quarterly report, 25 Apr. - 24 Jul. 1966
Cadmium sulfide-thin film large area photovoltaic solar energy converter - plastic substrate cell fabrication and stability testing under various conditions of temperature and humidit
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