Difference between revisions of "User:Tohline/Appendix/Equation templates"
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* [LL75] '''Laundau, L. D. & Lifshitz, E. M.''' 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press) | * [LL75] '''Laundau, L. D. & Lifshitz, E. M.''' 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press) | ||
** <span id="LL75note_Euler01">EQ_Euler01</span> — In the Euler equation, LL75 do not initially include a source term to account for a gradient in the Newtonian gravitational potential, {{User:Tohline/Math/VAR_NewtonianPotential01}}; a term representing acceleration due to gravity, <math>\vec{g} = -\nabla\Phi</math>, is introduced in Eq.(2.4), but in LL75 this is intended primarily to describe gravity at the surface of the Earth. | ** <span id="LL75note_Euler01">EQ_Euler01</span> — In the Euler equation, LL75 do not initially include a source term to account for a gradient in the Newtonian gravitational potential, {{User:Tohline/Math/VAR_NewtonianPotential01}}; a term representing acceleration due to gravity, <math>\vec{g} = -\nabla\Phi</math>, is introduced in Eq.(2.4), but in LL75 this is intended primarily to describe gravity at the surface of the Earth. | ||
** <span id="LL75note_Poisson01">EQ_Poisson01</span> — In LL75, the symbol <math>\Delta</math>, rather than <math>\nabla^2</math>, is used to represent the Laplacian spatial operator. | |||
* [BT87] '''Binney, J. & Tremaine, S.''' 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press) | * [BT87] '''Binney, J. & Tremaine, S.''' 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press) |
Revision as of 20:23, 24 January 2010
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Key Equations
To insert a given equation into any Wiki document, type ... |
Parallel References (Section & Eq. #) |
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Template_Name |
Resulting Equation |
C67 |
LL75 |
BT87 |
KW94 |
P00 |
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I: §8.5 |
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§I.2 |
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I: §8.5 |
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I: §8.5 |
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§I.3 |
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I: §10.2 |
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<math>~P = n_g k T</math> |
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§II.1 |
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I: §5.6 |
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<math>~P = (\gamma_\mathrm{g} - 1)\epsilon \rho </math> |
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Key Parallel Printed Reference Texts (spanning 5+ decades)
- [C67] Chandrasekhar, S. 1967 (originally, 1939), An Introduction to the Study of Stellar Structure (New York: Dover)
- EQ_EOSideal0A — In C67, the ideal gas equation of state is initially written in terms of the specific volume <math>~V</math>, instead of the mass density <math>~\rho</math>; also, it is initially assumed that <math>~\bar{\mu}</math> = 1. Both <math>~\rho</math> and <math>~\bar{\mu}</math> are introduced in §III.1, Eq.(5).
- [LL75] Laundau, L. D. & Lifshitz, E. M. 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)
- EQ_Euler01 — In the Euler equation, LL75 do not initially include a source term to account for a gradient in the Newtonian gravitational potential, <math>~\Phi</math>; a term representing acceleration due to gravity, <math>\vec{g} = -\nabla\Phi</math>, is introduced in Eq.(2.4), but in LL75 this is intended primarily to describe gravity at the surface of the Earth.
- EQ_Poisson01 — In LL75, the symbol <math>\Delta</math>, rather than <math>\nabla^2</math>, is used to represent the Laplacian spatial operator.
- [BT87] Binney, J. & Tremaine, S. 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press)
- [KW94] Kippenhahn, R. & Weigert, A. 1994, Stellar Structure and Evolution (New York: Springer-Verlag)
- [P00] Padmanabhan, T. 2000, Theoretical Astrophysics. Volume I: Astrophysical Processes (Cambridge: Cambridge University Press); and Padmanabhan, T. 2001, Theoretical Astrophysics. Volume II: Stars and Stellar Systems (Cambridge: Cambridge University Press)
- EQ_Poisson01 — See also Vol.I: §10.4, Eq.(10.58).
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