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==Step 1:== Following Rosseland, we adopt as a supplemental relation what we have [[SR/IdealGas#Consequential_Ideal_Gas_Relations|referred to elsewhere]] as, <div align="center"> <span id="ConservingMass:Lagrangian"><font color="#770000">'''Form B'''</font></span><br /> of the Ideal Gas Equation of State, {{Math/EQ_EOSideal02}} </div> where, for our purposes, we assume that {{Math/MP_AdiabaticIndex}} is independent of space and time. Plugging the function, <math>~\epsilon(P,\rho)</math>, that is defined by this equation of state into the adiabatic form of the 1<sup>st</sup> law of thermodynamics leads to the relations (see, respectively, Rosseland's equations 2.8 and 2.9), <div align="center"> <table border="0" cellpadding="5" align="center"> <tr> <td align="right"> <math>~\frac{dP}{dt}</math> </td> <td align="center"> <math>~=</math> </td> <td align="left"> <math>~\frac{\gamma_g P}{\rho} \frac{d\rho}{dt} \, ,</math> </td> </tr> </table> </div> and, <div align="center"> <table border="0" cellpadding="5" align="center"> <tr> <td align="right"> <math>~\frac{P}{P_0} </math> </td> <td align="center"> <math>~=</math> </td> <td align="left"> <math>~\biggl( \frac{\rho}{\rho_0}\biggr)^{\gamma_g} \, ,</math> </td> </tr> </table> </div> where <math>~P_0</math> and <math>~\rho_0</math> are independent of time. We note for later use that, when the equation of continuity — as written in its original vector-operator form — is combined with this last differential form of the 1<sup>st</sup> law of thermodynamics, we can write, <div align="center"> <table border="0" cellpadding="5" align="center"> <tr> <td align="right"> <math>~\frac{dP}{dt}</math> </td> <td align="center"> <math>~=</math> </td> <td align="left"> <math>~- \gamma_g P \nabla\cdot \vec{v} \, .</math> </td> </tr> </table> </div>
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