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Rotationally Flattened White Dwarfs
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Introduction
As we have reviewed in an accompanying discussion, Chandrasekhar (1935) was the first to construct models of spherically symmetric stars using the barotropic equation of state appropriate for a degenerate electron gas. In so doing, he demonstrated that the maximum mass of an isolated, nonrotating white dwarf is <math>M_3 = 1.44 (\mu_e/2)M_\odot</math>. A concise derivation of <math>~M_3</math> is presented in Chapter XI of Chandrasekhar (1967).
Something catastrophic should happen if mass is greater than <math>~M_3</math>. What will rotation do? Presumably it can increase the limiting mass.
Solution Strategy
Our Approach
When the stated objective is to construct steadystate equilibrium models of rotationally flattened, axisymmetric configurations, the accompanying introductory chapter shows how the overarching set of principal governing equations can be reduced in form to the following set of three coupled PDEs (expressed either in terms of cylindrical or spherical coordinates):
Table 1: Simplified Set of Three Coupled PDEs  

Cylindrical Coordinate Base  Spherical Coordinate Base  
Poisson Equation
The Two Relevant Components of the

Poisson Equation
The Two Relevant Components of the

This set of simplified governing relations must then be supplemented by a specification of: (a) a barotropic equation of state, <math>~P(\rho)</math>; and (b) the equilibrium configurations's radial specific angular momentum profile <math>~j(\varpi)</math>. How does this recommended modeling approach compare to the approach outlined by Ostriker, Bodenheimer & LyndenBell (1966) and further detailed and executed by J. P. Ostriker & P. Bodenheimer (1968)?
Approach Outlined by OBL66
 J. P. Ostriker, P. Bodenheimer & D. LyndenBell (1966; hereinafter OBL66), Phys. Rev. Letters, 17, 816: Equilibrium Models of Differentially Rotating ZeroTemperature Stars
… work by Roxburgh (1965, Z. Astrophys., 62, 134), Anand (1965, Proc. Natl. Acad. Sci. U.S., 54, 23), and James (1964, ApJ, 140, 552) shows that the [Chandrasekhar (1931, ApJ, 74, 81)] mass limit <math>~M_3</math> is increased by only a few percent when uniform rotation is included in the models, … In this Letter we demonstrate that whitedwarf models with masses considerably greater than <math>~M_3</math> are possible if differential rotation is allowed … models are based on the physical assumption of an axially symmetric, completely degenerate, selfgravitating fluid, in which the effects of viscosity, magnetic fields, meridional circulation, and relativistic terms in the hydrodynamical equations have been neglected. 
Their Equation (4)
One can immediately appreciate that, independent of the chosen coordinate base, the first expression listed among our trio of governing PDEs derives from the differential representation of the Poisson equation as discussed elsewhere and as has been reprinted here as Table 2.
Table 2: Poisson Equation  

Integral Representation  Differential Representation  


OBL66 chose, instead, to use the integral representation of the Poisson equation to evaluate the gravitational potential; specifically, they write,
<math>~ \Phi_g(\vec{x})</math> 
<math>~=</math> 
<math>~ G \int \frac{\rho(\vec{x}^{~'})}{\vec{x}^{~'}  \vec{x}} d^3x^' \, .</math> 
OBL66, p. 817, Eq. (4) 
(Note that, in defining <math>~\Phi_g</math>, OBL66 have adopted a sign convention for the gravitational potential that is the opposite of ours; that is, <math>~\Phi_g =  \Phi</math>.)
Their Equations (3) & (5)
The two relevant components of the Euler equation that are identified, above, result from imposing a steadystate condition on the,
Eulerian Representation
of the Euler Equation,
<math>~\cancel{\frac{\partial \vec{v}}{\partial t} } + (\vec{v} \cdot \nabla)\vec{v}</math> 
<math>~=</math> 
<math>~  \frac{1}{\rho} \nabla P  \nabla \Phi \, , </math> 
and adopting a steadystate rotational velocity field in which the angular velocity is either constant or is only a function of the cylindricalcoordinate radius, <math>~\varpi</math>; that is,
<math>~\vec{v} = \hat{e}_\varphi [v_\varphi] = \hat{e}_\varphi [\varpi \dot\varphi (\varpi)] \, .</math>
As we have demonstrated in an accompanying discussion, for any of a number of astrophysically relevant simple rotation profiles of this form, the convective operator on the lefthand side of this steadystate Euler equation gives (most conveniently written here in a cylindricalcoordinate base),
<math>~(\vec{v} \cdot \nabla)\vec{v}</math> 
<math>~=</math> 
<math>~~\hat{e}_\varpi \biggl[\frac{v_\varphi^2}{\varpi} \biggr] = ~\hat{e}_\varpi \biggl[ \varpi {\dot\varphi}^2(\varpi) \biggr] = ~\hat{e}_\varpi \biggl[\frac{j^2(\varpi)}{\varpi^3} \biggr] \, ,</math> 
where, <math>~j \equiv \varpi^2 \dot\varphi</math> is the (radially dependent) specific angular momentum measured relative to the symmetry (rotation) axis. As we have pointed out in an accompanying discussion, this last expression can be rewritten in terms of the gradient of a scalar (centrifugal) potential; specifically,
<math>~(\vec{v} \cdot \nabla) \vec{v}</math> 
<math>~\rightarrow</math> 
<math>~\nabla \Psi \, ,</math> 
if the centrifugal potential is defined such that,
<math>~\Psi(\varpi)</math> 
<math>~\equiv</math> 
<math>~ \int_0^\varpi \frac{j^2(\varpi^')}{(\varpi^')^3} d\varpi^' \, .</math> 
OBL66, p. 817, Eq. (5) 
(Note that OBL66 adopted a sign convention for the centrifugal potential that is the opposite of ours; that is, <math>~\Phi_c =  \Psi</math>.) Hence, assuming that our intent is to construct a rotationally flattened equilibrium configuration whose rotation profile is of the form, <math>~\vec{v} = \hat{e}_\varphi [\varpi \dot\varphi (\varpi)] </math>, the steadystate Euler equation can be rewritten as,
<math>~\frac{1}{\rho} \nabla P</math> 
<math>~=</math> 
<math>~  \nabla \Phi  \nabla \Psi \, . </math> 
OBL66, p. 817, Eq. (3) 
Their Adopted AngularMomentum Distribution
In what follows, text that has been extracted directly from p. 817 of OBL66 is presented using a dark green font.
"The angularvelocity distribution in the model is determined through the specification of a distribution of angular momentum per unit mass <math>~j(m)</math>, where <math>~m</math> is a Lagrangian coordinate equal to the fraction of the total mass interior to a cylindrical surface around the axis of rotation. The specification of <math>~j(m)</math> rather than <math>~\dot\varphi(\varpi)</math> permits the construction of equilibrium models for a given choice of [total] angular momentum <math>~J</math>. The angularmomentum distribution chosen for the computed models is that of a uniformly rotating polytrope of index <math>~\tfrac{3}{2}</math>."
Later papers refer to models with OBL66's specified angular momentum profile as belonging to an <math>~n^' = \tfrac{3}{2}</math> sequence. It cannot be described by a closedform analytic expression. But, as a point of reference and drawing from Stoeckly's (1965) work, in an accompanying discussion we derive the analytic expression for the angular momentum distribution of models that lie along a socalled <math>~n^' = 0</math> sequence.
Their Adopted Barotropic Equation of State
Because they were interested in constructing equilibrium models of rotationally flattened white dwarfs, OBL66 chose a barotropic equation of state that describes a zerotemperature Fermi (degenerate electron) gas. As has been documented in our accompanying discussion of barotropic equations of state, the set of key relations that define this equation of state is,
<math>~P_\mathrm{deg} = A_\mathrm{F} F(\chi) </math> 

where: <math>F(\chi) \equiv \chi(2\chi^2  3)(\chi^2 + 1)^{1/2} + 3\sinh^{1}\chi</math> 

and: 
<math>\chi \equiv (\rho/B_\mathrm{F})^{1/3}</math> 
OBL66, p. 817, Eq. (2)
As we also have reviewed elsewhere, the Chandrasekhar limiting mass that is associated with this equation of state in nonrotating stars is given by the expression,
<math> \frac{M_\mathrm{Ch}}{M_\odot} = \frac{5.742}{\mu_e^2} .
</math>OBL66, p. 816, Eq. (1)
Further Implementation by OB68
If we define an effective potential,
<math>~\Phi_\mathrm{eff}</math> 
<math>~\equiv</math> 
<math>~\Phi + \Psi \, ,</math> 
and recall that, for a barotropic equation of state, we can make the substitution, <math>~\nabla P \rightarrow \rho\nabla H</math>, where <math>~H</math> is the fluid enthalpy, then OBL66's hydrostatic balance equation — their equation (3) — can be rewritten as,
<math>~\nabla [H + \Phi_\mathrm{eff} ]</math> 
<math>~=</math> 
<math>~0 </math> 
<math>~\Rightarrow</math> 
<math>~H + \Phi_\mathrm{eff}</math> 
<math>~=</math> 
<math>~C_B \, , </math> 
where, <math>~C_B</math> is a constant (i.e., independent of position). Rotationally flattened, steadystate (equilibrium) configurations can be constructed by finding spatial density distributions that simultaneously satisfy the Poisson equation and this deceptively simple algebraic relation. Ostriker & Bodenheimer (1968; hereinafter, OB68) used this "selfconsistent field" technique to obtain models of rotationally flattened white dwarfs; it is a technique of choice that we broadly promote as well.
In the specific case of a zerotemperature Fermi (degenerate electron) gas — see our related discussion of barotropic structures — to within an additive constant, the enthalpy associated with <math>~P_\mathrm{deg}</math> is,
<math>~H</math> 
<math>~=</math> 
<math>~ \frac{8A_\mathrm{F}}{B_\mathrm{F}} \biggl[ (1 + \chi^2 )^{1 / 2} \biggr] </math> 
<math>~=</math> 
<math>~ \frac{8A_\mathrm{F}}{B_\mathrm{F}} \biggl\{ \biggl[1 + \biggl(\frac{\rho}{B_\mathrm{F}}\biggr)^{2/3} \biggr]^{1 / 2} \biggr\} \, . </math> 

OB68, p. 1090, Eq. (4) 
Note that, using this expression, the enthalpy at the surface <math>~(\rho = 0)</math> is <math>~H_s = 8A_\mathrm{F}/B_\mathrm{F}</math>. (Our tabulated expression for the enthalpy has been shifted by this constant value so that the enthalpy naturally goes to zero at the surface.) If we use <math>~\Phi_\mathrm{eff,s}</math> to denote the surface value of the effective potential, the constant in the algebraic hydrostaticbalance expression must be,
<math>~C_B</math> 
<math>~=</math> 
<math>~H_s + \Phi_\mathrm{eff,s}</math> 
Then, at every other spatial location, <math>~\vec{x}</math>, we must have,
<math>~H(\vec{x})  H_s + \Phi_\mathrm{eff}(\vec{x})  \Phi_\mathrm{eff,s}</math> 
<math>~=</math> 
<math>~0</math> 
<math>~\Rightarrow ~~~ \frac{8A_\mathrm{F}}{B_\mathrm{F}} \Biggl[ \biggl\{ \biggl[1 + \biggl(\frac{\rho(\vec{x})}{B_\mathrm{F}}\biggr)^{2/3} \biggr]^{1 / 2} \biggr\}  1 \Biggr]</math> 
<math>~=</math> 
<math>~ \Phi_\mathrm{eff}(\vec{x}) + \Phi_\mathrm{eff,s}</math> 
<math>~\Rightarrow ~~~ \frac{\rho(\vec{x})}{B_\mathrm{F}} </math> 
<math>~=</math> 
<math>~ \Biggl[ \biggl\{ \frac{B_\mathrm{F}}{8A_\mathrm{F}} \biggl[ \Phi_\mathrm{eff}(\vec{x}) + \Phi_\mathrm{eff,s}\biggr] + 1 \biggr\}^2  1 \Biggr]^{3/2} \, . </math> 
OB68, p. 1090, Eq. (5) 
(Note that, as with OBL66, a different sign convention was adopted by OB68 for the effective potential than we have used; that is, <math>~\mathfrak{B} =  \Phi_\mathrm{eff}</math>.)
See Also
© 2014  2021 by Joel E. Tohline 