Difference between revisions of "User:Tohline/Appendix/Equation templates"

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I: &#167;10.2<br /> (10.1)
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&#167;II.1<br /> (1) <br />[http://www.vistrails.org/index.php/User:Tohline/Appendix/Equation_templates#C67note01  Note]
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''<font size="+2" color="darkblue">
''<font size="+2" color="darkblue">
Key Parallel References (spanning 5+ decades)
Key Parallel Reference Texts (spanning 5+ decades)
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* [C67] Chandrasekhar, S. 1967 (originally, 1939) An Introduction to the Study of Stellar Structure (New York: Dover)
* [C67] Chandrasekhar, S. 1967 (originally, 1939) An Introduction to the Study of Stellar Structure (New York: Dover)
** <span id="C67note01">EQ_EOSideal0A</span> &#8212; In C67, the ideal gas equation of state is written in terms of the specific volume {{User:Tohline/Math/VAR_SpecificVolume01}}, instead of the mass density {{User:Tohline/Math/VAR_Density01}}; also, it is assumed that {{User:Tohline/Math/MP_MeanMolecularWeight}} = 1.
* [LL75] Laundau, L. D. &amp; Lifshitz, E. M. 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)
* [LL75] Laundau, L. D. &amp; Lifshitz, E. M. 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)
* [BT87] Binney, J. &amp; Tremaine, S. 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press)
* [BT87] Binney, J. &amp; Tremaine, S. 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press)

Revision as of 19:28, 24 January 2010

Whitworth's (1981) Isothermal Free-Energy Surface
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Key Equations

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

LSU Key.png

<math>\frac{d\rho}{dt} + \rho \nabla \cdot \vec{v} = 0</math>

 

I: §8.5
(8.45)

EQ_Euler01

LSU Key.png

<math>\frac{d\vec{v}}{dt} = - \frac{1}{\rho} \nabla P - \nabla \Phi</math>

 

I: §8.5
(8.48)

EQ_FirstLaw01

LSU Key.png

<math>T \frac{ds}{dt} = \frac{d\epsilon}{dt} + P \frac{d}{dt} \biggl(\frac{1}{\rho}\biggr)</math>

 

I: §8.5
(8.53)

EQ_Poisson01

LSU Key.png

<math>\nabla^2 \Phi = 4\pi G \rho</math>

 

I: §10.2
(10.1)

EQ_EOSideal00

<math>~P = n_g k T</math>

 

EQ_EOSideal0A

LSU Key.png

<math>~P_\mathrm{gas} = \frac{\Re}{\bar{\mu}} \rho T</math>

§II.1
(1)
Note

 

I: §5.6
(5.91)

EQ_EOSideal02

<math>~P = (\gamma_\mathrm{g} - 1)\epsilon \rho </math>

 

 

Key Parallel 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 written in terms of the specific volume <math>~V</math>, instead of the mass density <math>~\rho</math>; also, it is assumed that <math>~\bar{\mu}</math> = 1.
  • [LL75] Laundau, L. D. & Lifshitz, E. M. 1975 (originally, 1959), Fluid Mechanics (New York: Pergamon Press)
  • [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)

 

Whitworth's (1981) Isothermal Free-Energy Surface

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