User:Tohline/Appendix/Equation templates

Key Equations

Each of the equations displayed in the Table, below, encapsulates a physical concept that is fundamental to our understanding of — and, hence our discussion of — the structure, stability, and dynamics of self-gravitating systems. The pervasiveness of these physical concepts throughout astrophysics is reflected in the fact that the same equations — perhaps written in slightly different forms — appear in numerous published texts. When attempting to understand the physical concept that is associated with any one of these mathematical relations, it can be helpful to read how and in what context different authors introduce the expressoin. The Table, below, offers a guide to some of these parallel discussions that have appeared in published texts over the past 5+ decades.

To insert a given equation into any Wiki document, type ... {{ User:Tohline/Math/Template_Name }}		Parallel References (Section & Eq. #)
Template_Name	Resulting Equation	C67	LL75	BT87	KW94	P00
EQ_Continuity01	<math>\frac{d\rho}{dt} + \rho \nabla \cdot \vec{v} = 0</math>		§I.1 (1.2) Note			I: §8.5 (8.45)
EQ_Euler01	<math>\frac{d\vec{v}}{dt} = - \frac{1}{\rho} \nabla P - \nabla \Phi</math>		§I.2 (2.1) Note			I: §8.5 (8.48)
EQ_FirstLaw01	<math>T \frac{ds}{dt} = \frac{d\epsilon}{dt} + P \frac{d}{dt} \biggl(\frac{1}{\rho}\biggr)</math>		§I.2 (2.5) Note			I: §8.5 (8.53)
EQ_Poisson01	<math>\nabla^2 \Phi = 4\pi G \rho</math>		§I.3 (3.5) Note			I: §10.2 (10.1) Note
EQ_EOSideal00	<math>~P = n_g k T</math>
EQ_EOSideal0A	<math>~P_\mathrm{gas} = \frac{\Re}{\bar{\mu}} \rho T</math>	§II.1 (1) Note	§IX.80 (80.8)			I: §5.6 (5.91)
EQ_EOSideal02	<math>~P = (\gamma_\mathrm{g} - 1)\epsilon \rho </math>

 

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_Continuity01 — LL75 present the Eulerian, rather than the Lagrangian form of the Continuity equation.
  • 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_FirstLaw01 — LL75's Eq.(2.5) must be combined with their discussion of what they refer to as the familiar thermodynamic relation (between LL75 Eqs. 2.8 and 2.9) in order to appreciate the similarity with our expression.
  • 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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