G. Ogilvie. (2016)cite arxiv:1604.03835Comment: 94 pages, 23 figures, to be published in the Journal of Plasma Physics (JPP Lecture Notes).
Abstract
These lecture notes and example problems are based on a course given at the
University of Cambridge in Part III of the Mathematical Tripos.
Fluid dynamics is involved in a very wide range of astrophysical phenomena,
such as the formation and internal dynamics of stars and giant planets, the
workings of jets and accretion discs around stars and black holes, and the
dynamics of the expanding Universe. Effects that can be important in
astrophysical fluids include compressibility, self-gravitation and the
dynamical influence of the magnetic field that is 'frozen in' to a highly
conducting plasma.
The basic models introduced and applied in this course are Newtonian gas
dynamics and magnetohydrodynamics (MHD) for an ideal compressible fluid. The
mathematical structure of the governing equations and the associated
conservation laws are explored in some detail because of their importance for
both analytical and numerical methods of solution, as well as for physical
interpretation. Linear and nonlinear waves, including shocks and other
discontinuities, are discussed. The spherical blast wave resulting from a
supernova, and involving a strong shock, is a classic problem that can be
solved analytically. Steady solutions with spherical or axial symmetry reveal
the physics of winds and jets from stars and discs. The linearized equations
determine the oscillation modes of astrophysical bodies, as well as determining
their stability and their response to tidal forcing.
%0 Generic
%1 ogilvie2016lecture
%A Ogilvie, Gordon I.
%D 2016
%K dynamics fluid notes
%T Lecture notes: Astrophysical fluid dynamics
%U http://arxiv.org/abs/1604.03835
%X These lecture notes and example problems are based on a course given at the
University of Cambridge in Part III of the Mathematical Tripos.
Fluid dynamics is involved in a very wide range of astrophysical phenomena,
such as the formation and internal dynamics of stars and giant planets, the
workings of jets and accretion discs around stars and black holes, and the
dynamics of the expanding Universe. Effects that can be important in
astrophysical fluids include compressibility, self-gravitation and the
dynamical influence of the magnetic field that is 'frozen in' to a highly
conducting plasma.
The basic models introduced and applied in this course are Newtonian gas
dynamics and magnetohydrodynamics (MHD) for an ideal compressible fluid. The
mathematical structure of the governing equations and the associated
conservation laws are explored in some detail because of their importance for
both analytical and numerical methods of solution, as well as for physical
interpretation. Linear and nonlinear waves, including shocks and other
discontinuities, are discussed. The spherical blast wave resulting from a
supernova, and involving a strong shock, is a classic problem that can be
solved analytically. Steady solutions with spherical or axial symmetry reveal
the physics of winds and jets from stars and discs. The linearized equations
determine the oscillation modes of astrophysical bodies, as well as determining
their stability and their response to tidal forcing.
@misc{ogilvie2016lecture,
abstract = {These lecture notes and example problems are based on a course given at the
University of Cambridge in Part III of the Mathematical Tripos.
Fluid dynamics is involved in a very wide range of astrophysical phenomena,
such as the formation and internal dynamics of stars and giant planets, the
workings of jets and accretion discs around stars and black holes, and the
dynamics of the expanding Universe. Effects that can be important in
astrophysical fluids include compressibility, self-gravitation and the
dynamical influence of the magnetic field that is 'frozen in' to a highly
conducting plasma.
The basic models introduced and applied in this course are Newtonian gas
dynamics and magnetohydrodynamics (MHD) for an ideal compressible fluid. The
mathematical structure of the governing equations and the associated
conservation laws are explored in some detail because of their importance for
both analytical and numerical methods of solution, as well as for physical
interpretation. Linear and nonlinear waves, including shocks and other
discontinuities, are discussed. The spherical blast wave resulting from a
supernova, and involving a strong shock, is a classic problem that can be
solved analytically. Steady solutions with spherical or axial symmetry reveal
the physics of winds and jets from stars and discs. The linearized equations
determine the oscillation modes of astrophysical bodies, as well as determining
their stability and their response to tidal forcing.},
added-at = {2016-04-14T10:06:25.000+0200},
author = {Ogilvie, Gordon I.},
biburl = {https://www.bibsonomy.org/bibtex/2ad8e3b5587a76b9d81998542c7a48a30/miki},
description = {[1604.03835] Lecture notes: Astrophysical fluid dynamics},
interhash = {16d4d8f8c8c93af6abe3766c46cd1460},
intrahash = {ad8e3b5587a76b9d81998542c7a48a30},
keywords = {dynamics fluid notes},
note = {cite arxiv:1604.03835Comment: 94 pages, 23 figures, to be published in the Journal of Plasma Physics (JPP Lecture Notes)},
timestamp = {2016-04-14T10:06:25.000+0200},
title = {Lecture notes: Astrophysical fluid dynamics},
url = {http://arxiv.org/abs/1604.03835},
year = 2016
}