Editing Apps/OstrikerBodenheimerLyndenBell66 (section)

====Their Adopted Barotropic Equation of State====

Because they were interested in constructing equilibrium models of rotationally flattened white dwarfs, [https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract OBL66] chose a barotropic equation of state that describes a ''zero-temperature Fermi (degenerate electron) gas''.  As has been documented in our [[SR#Barotropic_Structure|accompanying discussion of barotropic equations of state]], the set of key relations that define this equation of state is,

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{{Math/EQ_ZTFG01}}
Reference (original): [http://adsabs.harvard.edu/abs/1935MNRAS..95..207C S. Chandraskehar (1935)]<p></p>
[https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract OBL66], p. 817, Eq. (2)
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As we also have [[SSC/Structure/WhiteDwarfs#ChandrasekharMass|reviewed elsewhere]], the ''Chandrasekhar limiting mass'' that is associated with this equation of state in ''nonrotating'' stars is given by the expression,
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<math>
\frac{M_\mathrm{Ch}}{M_\odot} = \frac{5.742}{\mu_e^2} .
</math><p></p>
[https://ui.adsabs.harvard.edu/abs/1966PhRvL..17..816O/abstract OBL66], p. 816, Eq. (1)
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