Editing Appendix/EquationTemplates (section)

=Key Parallel References (printed texts spanning 5+ decades)=


* [<b><font color="red">C67</font></b>] [http://adsabs.harvard.edu/abs/1967aits.book.....C '''Chandrasekhar, S.''' 1967] (originally, 1939), An Introduction to the Study of Stellar Structure (New York: Dover) 
** <span id="C67note_EOSideal0A">EQ_EOSideal0A</span> &#8212; In C67, the ideal gas equation of state is initially written in terms of the specific volume {{Template:Math/VAR_SpecificVolume01}}, instead of the mass density {{Template:Math/VAR_Density01}}; also, it is initially assumed that {{Template:Math/MP_MeanMolecularWeight}} = 1.  Both {{Template:Math/VAR_Density01}} and {{Template:Math/MP_MeanMolecularWeight}} are introduced in &#167;III.1, Eq.(5). 
** <span id="C67note_SSLaneEmden01">EQ_SSLaneEmden01</span> &#8212; At the end of his Chapter IV, C67 writes an extensive history of the earliest work on stellar structure pointing especially the origins of the so-called Lane-Emden equation.  He points out, for example, that [http://gallica.bnf.fr/ark:/12148/bpt6k152556/f340.image.r=Annalen%20der%20Physic.langEN Ritter (1880)] actually published this governing differential equation prior to Emden. 


* [<b><font color="red">LL75</font></b>] [http://adsabs.harvard.edu/abs/1959flme.book.....L '''Laundau, L. D. &amp; Lifshitz, E. M.''' 1975 (originally, 1959)], Fluid Mechanics (New York: Pergamon Press)
** <span id="LL75note_Continuity01">EQ_Continuity01</span> &#8212; LL75 present the Eulerian, rather than the Lagrangian form of the Continuity equation.
** <span id="LL75note_Euler01">EQ_Euler01</span> &#8212; In the Euler equation, LL75 do not initially include a source term to account for a gradient in the Newtonian gravitational potential, {{Template: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_FirstLaw01">EQ_FirstLaw01</span> &#8212; 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.
** <span id="LL75note_Poisson01">EQ_Poisson01</span> &#8212; In LL75, the symbol <math>\Delta</math>, rather than <math>\nabla^2</math>, is used to represent the Laplacian spatial operator.
** <span id="LL75note_EOSideal0A">EQ_EOSideal0A</span> &#8212; In LL75, the ideal gas equation of state is written in terms of the specific volume {{Template:Math/VAR_SpecificVolume01}}, as well as in terms of the mass density {{Template:Math/VAR_Density01}}.


* [<b><font color="red">ST83</font></b>] [http://adsabs.harvard.edu/abs/1983bhwd.book.....S '''Shapiro, S. L. &amp; Teukolsky, S. A.''' 1983], Black Holes, White Dwarfs, and Neutron Stars:  The Physics of Compact Objects (New York: John Wiley &amp; Sons); republished in 2004 by WILEY-VCH Verlag GmbH &amp; Co. KGaA
** <span id="ST83note_Euler01">EQ_Continuity01</span> &#8212; ST83 present the Eulerian, rather than the Lagrangian form of the Continuity equation. 


* [<b><font color="red">H87</font></b>] [http://adsabs.harvard.edu/abs/1987stme.book.....H '''Huang, K.''' 1987] (originally 1963), Statistical Mechanics (New York: John Wiley &amp; Sons)
** <span id="H87note_Euler01">EQ_Continuity01</span> &#8212; H87 presents the Eulerian, rather than the Lagrangian form of the Continuity equation, and the variable <math>\vec{u}</math> is used instead of {{Template:Math/VAR_VelocityVector01}} to represent the velocity.
** <span id="H87note_Continuity01">EQ_Euler01</span> &#8212; H87 presents the Eulerian, rather than the Lagrangian form of the Euler equation, and the variable <math>\vec{u}</math> is used instead of {{Template:Math/VAR_VelocityVector01}} to represent the velocity. Furthermore, to match the source term in our version of the Euler equation, we must set H87's applied acceleration, <math>\vec{F}/m = -\nabla</math>{{Template:Math/VAR_NewtonianPotential01}}.
** <span id="H87note_FirstLaw01">EQ_FirstLaw01</span> &#8212; H87 begins a discussion of the 1<sup>st</sup> Law of Thermodynamics in the first section of the first chapter, but it does not appear in the form we present (relevant for a "dilute gas") until Eq.(4.31).


* [<b><font color="red">BT87</font></b>] '''Binney, J. &amp; Tremaine, S.''' 1987, Galactic Dynamics (Princeton, NJ: Princeton University Press)


* [<b><font color="red">KW94</font></b>] '''Kippenhahn, R. &amp; Weigert, A.''' 1994, Stellar Structure and Evolution (New York: Springer-Verlag)
** <span id="KW94note_Continuity01">EQ_Continuity01</span> &#8212; KW94 present the Eulerian, rather than the Lagrangian form of the Continuity equation.
** <span id="KW94note_FirstLaw01">EQ_FirstLaw01</span> &#8212; In KW94, the symbol <math>u</math> instead of {{Template:Math/VAR_SpecificInternalEnergy01}} is used to represent the specific internal energy.
** <span id="KW94note_EOSideal0A">EQ_EOSideal0A</span> &#8212; In KW94, the ideal gas equation of state is actually first introduced in &#167;2.2, Eq.(27), but it is seriously discussed in Chapter 13.  KW94 provide a particularly nice explanation of how to calculate the model parameter, {{Template:Math/MP_MeanMolecularWeight}}.
** <span id="KW94note_SShydrostaticBalance">EQ_SShydrostaticBalance01</span> &#8212; In KW94, the hydrostatic balance equation is expressed in terms of <math>dP/dM_r</math> instead of <math>dP/dr</math>; and the second term on the right-hand-side allows for a net radial acceleration. 


* [<b><font color="red">HK94</font></b>] '''Hansen, C. J. &amp; Kawaler, S. D.''' 1994, Stellar Interiors:  Physical Principles, Structure, and Evolution (New York: Springer)


* [<b><font color="red">P00</font></b>] '''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)
** <span id="P00note_Poisson01">EQ_Poisson01</span> &#8212; See also Vol.I: &#167;10.4, Eq.(10.58).


* [<b><font color="red">BLRY07</font></b>] <span id="BLRY07">'''Bodenheimer, P., Laughlin, G. P., R&oacute;&#380;yczka, M. &amp; Yorke, H. W.''' 2007,</span> Numerical Methods in Astrophysics  <font size="-1">An Introduction</font> (New York: Taylor &amp; Francis)