Difference between revisions of "User:Tohline/PGE"
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In the next-to-last equation, {{User:Tohline/Math/VAR_SpecificInternalEnergy01}} is the specific internal energy of the gas, and in the last expression, {{User:Tohline/Math/C_GravitationalConstant}} is the Newtonian gravitational constant. | |||
These differential equations relate the time, t, and spatial, <math>\vec{x}</math>, variation of the principal variables to one another in a physically consistent fashion. By restricting our discussions to physical systems that are governed by this set of equations, for the most part '''we will be considering the structure, stability, and dynamical behavior of compressible, inviscid fluid systems that are self-gravitating.''' We will assume that no electromagnetic forces act on the fluid (''e.g.,'' the effects of magnetic fields on an ionized plasma fluid will not be considered) and, in the absence of dynamically generated shocks, we will assume that all compressions and rarefactions occur adiabatically. | |||
To complete the description of any specific astrophysical system, this set of differential equations must be supplemented by additional relations – for example a relationship between {{User:Tohline/Math/VAR_Pressure01}} and {{User:Tohline/Math/VAR_SpecificInternalEnergy01}} – which (at least in the context of this H_Book) usually will be algebraic expressions motivated by the specific physics that is relevant to the chosen system. | |||
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Revision as of 01:03, 22 January 2010
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Principal Governing Equations
According to the eloquent discussion of the broad subject of Fluid Mechanics presented by Landau and Lifshitz (1975), the state of a moving fluid is determined by five quantities: the three components of the velocity <math>~\vec{v}</math> and, for example, the pressure <math>~P</math> and the density <math>~\rho</math> . For our discussions of astrophysical fluid systems throughout this Hypertext Book [H_Book], we will add to this the gravitational potential <math>~\Phi</math>. Accordingly, a complete system of equations of fluid dynamics should be six in number. For an ideal fluid these are:
Euler's Equation
(Momentum Conservation)
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<math>\frac{d\vec{v}}{dt} = - \frac{1}{\rho} \nabla P - \nabla \Phi</math> |
Equation of Continuity
(Mass Conservation)
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<math>\frac{d\rho}{dt} + \rho \nabla \cdot \vec{v} = 0</math> |
Adiabatic Form of the
First Law of Thermodynamics
(Specific Entropy Conservation)
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<math>T \frac{ds}{dt} = \frac{d\epsilon}{dt} + P \frac{d}{dt} \biggl(\frac{1}{\rho}\biggr)</math> |
Poisson Equation
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<math>\nabla^2 \Phi = 4\pi G \rho</math> |
In the next-to-last equation, <math>~\epsilon</math> is the specific internal energy of the gas, and in the last expression, <math>~G</math> is the Newtonian gravitational constant.
These differential equations relate the time, t, and spatial, <math>\vec{x}</math>, variation of the principal variables to one another in a physically consistent fashion. By restricting our discussions to physical systems that are governed by this set of equations, for the most part we will be considering the structure, stability, and dynamical behavior of compressible, inviscid fluid systems that are self-gravitating. We will assume that no electromagnetic forces act on the fluid (e.g., the effects of magnetic fields on an ionized plasma fluid will not be considered) and, in the absence of dynamically generated shocks, we will assume that all compressions and rarefactions occur adiabatically.
To complete the description of any specific astrophysical system, this set of differential equations must be supplemented by additional relations – for example a relationship between <math>~P</math> and <math>~\epsilon</math> – which (at least in the context of this H_Book) usually will be algebraic expressions motivated by the specific physics that is relevant to the chosen system.
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