SSC/VariationalPrinciple/Pt2

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Ledoux's Variational Principle[edit]


Part I:  Ledoux & Pekeris (1941)

 


Part II:  Exploratory Ideas

 


Related, Exploratory Ideas[edit]

Logarithmic Derivatives[edit]

Returning to our above discussion of the Ledoux & Walraven approach, we appreciate that the differential relation governing the Variational Principle is,

σ2ρr4ξ2

=

r4Γ1P(dξdr)2(3Γ14)r3ξ2(dPdr)ddr[r4Γ1Pξ(dξdr)]

ddr[r3Γ1Pξ2(dlnξdlnr)]

=

r4Γ1P(dξdr)2(3Γ14)r3ξ2(dPdr)σ2ρr4ξ2

 

=

ξ2{r2Γ1P(dlnξdlnr)2(3Γ14)r3(dPdr)σ2ρr4}

 

=

(rξ)2P{Γ1(dlnξdlnr)2(3Γ14)(dlnPdlnr)σ2ρr2P}

 

=

Γ1(rξ)2P{(dlnξdlnr)2α(dlnPdlnr)σ2ρr2Γ1P},

where,

α(34Γ1).

Pressure-Truncated Polytropes[edit]

Let's start with the integral expression derived in our discussion of the Ledoux & Walraven approach; insert the variable, x, in place of ξ; and adopt the boundary conditions,

r=0   at the center,

        along with        

P=Pe,   and  dlnxdlnr=3   at the surface (r = R).

That is, let's start with,

0Rσ2ρr4x2dr

=

0Rr4Γ1P(dxdr)2dr0R(3Γ14)r3x2(dPdr)dr+3Γ1PeR3xsurface2.

Via Generalized Normalization[edit]

Next, we'll divide through by the normalization energy, as defined in an accompanying discussion,

Enorm=PnormRnorm3=GMtot2Rnorm,

thereby making the integral relation dimensionless:

0

=

[RnormGMtot2]0Rσ2ρr4x2dr+[1PnormRnorm3]0Rr4Γ1P(dxdr)2dr[1PnormRnorm3]0R(3Γ14)r3x2(dPdr)dr+[PeR3PnormRnorm3]3Γ1xsurface2

 

=

[RnormR5ρc2Mtot2]0Rx2(σ2Gρc)(ρρc)(rR)4drR+[PcR3PnormRnorm3]0R(rR)4Γ1(PPc)[dxd(r/R)]2drR

 

 

[PcR3PnormRnorm3]0R(3Γ14)(rR)3x2[d(P/Pc)d(r/R)]drR+[PeR3PnormRnorm3]3Γ1xsurface2

 

=

[MMtot]2[(34π)ρcρ¯]2χ10Rx2(σ2Gρc)(ρρc)(rR)4drR+[PePnorm]3Γ1χ3xsurface2

 

 

+[PcPnorm]χ30R{(rR)4Γ1(PPc)[dxd(r/R)]2(3Γ14)(rR)3x2[d(P/Pc)d(r/R)]}drR,

where,

χRRnorm.

Note that we will ultimately insert the relation,

PcPnorm=[(34π)ρcρ¯(MMtot)]Γ1(RRnorm)3Γ1.

But, for the time being, dividing through by [Pc/Pnorm]χ3 gives,

0

=

[PcPnorm]1[MMtot]2[(34π)ρcρ¯]2χ40Rx2(σ2Gρc)(ρρc)(rR)4drR

 

 

+[PePc]3Γ1xsurface2+0R{(rR)4Γ1(PPc)[dxd(r/R)]2(3Γ14)(rR)3x2[d(P/Pc)d(r/R)]}drR,

Now let's focus on the second line of this integral energy relation, evaluating it for pressure-truncated polytropic configurations, in which case, Γ1(n+1)/n,

rRξξ~

        and        

PPcθn+1.

We have,

Second line of relation

=

[PePc]3Γ1xsurface2+0R{(rR)4Γ1(PPc)[dxd(r/R)]2(3Γ14)(rR)3x2[d(P/Pc)d(r/R)]}drR

 

=

[PePc][3(n+1)n]xsurface2+0ξ~{(ξξ~)4(n+1n)θn+1[dxdξ]2ξ~2(3nn)(ξξ~)3x2[dθn+1dξ]ξ~}dξξ~

 

=

[PePc][3(n+1)n]xsurface2+1nξ~30ξ~{(n+1)ξ4θn+1[dxdξ]2(3n)ξ3x2[dθn+1dξ]}dξ

 

=

[PePc][3(n+1)n]xsurface2+1nξ~30ξ~{(n+1)ξ4θn+1[dxdξ]2(n+1)(3n)ξ3x2θnθ'}dξ

 

=

[PePc][3(n+1)n]xsurface2+(n+1)nξ~30ξ~(32n)2ξθn{ξθ[(2n3)ξθndxdξ]2(3n)[(2n3)ξθnx]2θ'}dξ.

Now, let's examine how these terms combine if we guess the analytically defined eigenfunction that applies to marginally unstable, pressure-truncated polytropic configurations, namely,

x

=

3(n1)2n[1+(n3n1)θ'ξθn]

(2n3)ξθnx

=

[(n1)ξθn+(n3)θ']

dxdξ

=

[3(n3)2n]{θ'ξθnθ'ξ2θnn(θ')2ξθ(n+1)}

 

=

[3(n3)2n]1ξθn[θn+3θ'ξ+n(θ')2θ]

(2n3)ξθndxdξ

=

(3n)[θn+3θ'ξ+n(θ')2θ].

Hence,

Second line of relation

=

θ~n+1[3(n+1)n]{3(n1)2n[1+(n3n1)θ~'ξ~θ~n]}2

 

 

+32(n+1)(3n)22n3ξ~30ξ~ξθn{ξθ(3n)[θn+3θ'ξ+n(θ')2θ]2[(n1)ξθn+(n3)θ']2θ'}dξ

 

=

1ξ~2θ~n+1[33(n+1)22n3][(n1)ξ~θ~n+1+(n3)θ~θ~']2

 

 

+32(n+1)(3n)22n3ξ~30ξ~1θn+1{(3n)[ξθn+1+3θθ'+nξ(θ')2]2[(n1)ξθn+(n3)θ']2ξθθ'}dξ

 

=

1ξ~2θ~n+1[33(n+1)22n3][(n1)ξ~θ~n+1+(n3)θ~θ~']2

 

 

+32(n+1)(3n)222n3ξ~30ξ~1θn+1{[ξθn+1+3θθ'+nξ(θ')2]2+1(n3)[(n1)ξθn+(n3)θ']2ξθθ'}dξ

Note that, in this derivation, we have inserted the expressions:

[ξθn+1+3θθ'+nξ(θ')2][ξθn+1+3θθ'+nξ(θ')2]=ξ2θ2(n+1)+6ξθn+2θ'+2nξ2θn+1(θ')2+6nξθ(θ')3+n2ξ2(θ')4

1(n3)[(n1)ξθn+(n3)θ']2ξθ(θ')=[(n1)2(n3)]ξ3θ2n+1(θ')+2(n1)ξ2θn+1(θ')2+(n3)ξθ(θ')3

Directly to n = 5 Polytropic Configurations[edit]

Exact
Demonstration
of
Variational
Principle

0Rσ2ρr4x2dr

=

0Rr4Γ1P(dxdr)2dr0R(3Γ14)r3x2(dPdr)dr+3Γ1PeR3xsurface2

1R3Pc0Rσ2ρr4x2dr

=

0R(rR)4(n+1n)(PPc)[dxd(r/R)]2drR0R[3(n+1n)4](rR)3x2[d(P/Pc)d(r/R)]drR+3(n+1n)(PePc)xsurface2

 

=

0ξ~65(ξξ~)4θ6[dxd(ξ/ξ~)]2dξξ~0ξ~(25)(ξξ~)3x2[dθ6d(ξ/ξ~)]dξξ~+(185)θ~6xsurface2

 

=

1ξ~30ξ~(65)ξ4θ6[dxdξ]2dξ+1ξ~30ξ~(25)ξ3x2[dθ6dξ]dξ+(185)θ~6xsurface2

5ξ~32R3Pc0Rσ2ρr4x2dr

=

0ξ~3ξ4θ6[2ξ15]2dξ+0ξ~6ξ3[15ξ215]2θ5[dθdξ]dξ+9ξ~3θ~6[15ξ~215]2

 

=

(22352)0ξ~ξ6(33+ξ2)3dξ+(2352)0ξ~ξ3[15ξ2]2(33+ξ2)4[ξ3]dξ+(152)ξ~3(33+ξ~2)3[15ξ~2]2

 

=

(223252)0ξ~[ξ6(3+ξ2)3]dξ(23252)0ξ~[ξ4(15ξ2)2(3+ξ2)4]dξ+(3352)[ξ~3(15ξ~2)2(3+ξ~2)3]

53ξ~3232R3Pc0Rσ2ρr4x2dr

=

0ξ~[4ξ6(3+ξ2)2ξ4(15ξ2)2(3+ξ2)4]dξ+3[ξ~3(15ξ~2)2(3+ξ~2)3]

 

=

0ξ~{2ξ4[6ξ2+2ξ4152+30ξ2ξ4](3+ξ2)4}dξ+3[ξ~3(15ξ~2)2(3+ξ~2)3]

 

=

0ξ~{2ξ4[ξ4+36ξ2152](3+ξ2)4}dξ+3[ξ~3(15ξ~2)2(3+ξ~2)3]

 

=

[2ξ5(ξ215)(ξ2+3)3]0ξ~+3[ξ~3(15ξ~2)2(3+ξ~2)3]

 

=

[2ξ~5(ξ~215)(ξ~2+3)3]+3[ξ~3(15ξ~2)2(3+ξ~2)3]

 

=

2ξ~5(ξ~215)+3ξ~3(15ξ~2)2(ξ~2+3)3=5ξ~7120ξ~5+3352ξ~3(ξ~2+3)3,

which equals zero if ξ~=3. Hooray!!

For All Polytropic Indexes[edit]

Generalized Governing Integral Relation[edit]

Given that the derivation just completed works for the special case of n = 5, let's generalize it to all polytropic indexes

0Rσ2ρr4x2dr

=

0Rr4Γ1P(dxdr)2dr0R(3Γ14)r3x2(dPdr)dr+3Γ1PeR3xsurface2

R5ρcR3Pc0Rσ2(ρρc)(rR)4x2drR

=

0R(rR)4(n+1n)(PPc)[dxd(r/R)]2drR0R[3(n+1n)4](rR)3x2[d(P/Pc)d(r/R)]drR+3(n+1n)(PePc)xsurface2

R2ρcPc0ξ~σ2θn(ξξ~)4x2dξξ~

=

0ξ~(ξξ~)4(n+1n)θn+1[dxd(ξ/ξ~)]2dξξ~+0ξ~(n3n)(ξξ~)3x2[dθn+1d(ξ/ξ~)]dξξ~+3(n+1n)θ~n+1xsurface2

nR2ρc(n+1)ξ~2Pc0ξ~σ2θnξ4x2dξ

=

0ξ~ξ4θn+1[dxdξ]2dξ+0ξ~(n3)ξ3θnx2[dθdξ]dξ+3ξ~3θ~n+1xsurface2

nR2Gρc2(n+1)ξ~2Pc0ξ~(σ2Gρc)θnξ4x2dξ

=

0ξ~ξ2θn+1x2[ξxdxdξ]2dξ+0ξ~(n3)ξ2θn+1x2[ξθdθdξ]dξ+3ξ~3θ~n+1xsurface2

 

=

3ξ~3θ~n+1xsurface2+0ξ~ξ2θn+1x2{[ξxdxdξ]2+(n3)[ξθdθdξ]}dξ

For additional clarification, let's rewrite the leading coefficient on the lefthand-side of this expression.

LHS

=

nR2Gρc2(n+1)ξ~2Pc0ξ~(σ2Gρc)θnξ4x2dξ

 

=

[n(n+1)][GRnorm2Pnorm](RRnorm2)(ρcρ¯)2[3M4πR3]2(PnormPe)(PePc)[1ξ~2]0ξ~(σ2Gρc)θnξ4x2dξ

 

=

[n(n+1)][GMtot2PnormRnorm4](RnormR)4(ρcρ¯)2[(34π)MMtot]2(PnormPe)(PePc)[1ξ~2]0ξ~(σ2Gρc)θnξ4x2dξ

 

=

[n(n+1)](PnormPe)(RnormR)4(ξ~3θ~')2[(34π)MMtot]2[θ~n+1ξ~2]0ξ~(σ2Gρc)θnξ4x2dξ

Now, from an accompanying discussion, we know that, in equilibrium,

ReqRnorm

=

[(n+1)n(4π)]1/(n3)[MMtot](n1)/(n3)ξ~(ξ~2θ~)(1n)/(n3),

PePnorm

=

[(n+1)3(4π)1](n+1)/(n3)[MMtot]2(n+1)/(n3)θ~nn+1(ξ~2θ~)2(n+1)/(n3),

Hence,

(PePnorm)(ReqRnorm)4

=

{[(n+1)3(4π)1](n+1)[MMtot]2(n+1)θ~n(n+1)(n3)(ξ~2θ~)2(n+1)}1/(n3)

 

 

×{[(n+1)n(4π)][MMtot](n1)ξ~(n3)(ξ~2θ~)(1n)}4/(n3)

 

=

ξ~4θ~n(n+1){(n+1)3(n+1)(4π)(n1)[MMtot]2n2(ξ~2θ~)2n+2(n+1)4n(4π)4[MMtot](4n4)(ξ~2θ~)(44n)}1/(n3)

 

=

ξ~4θ~n(n+1){(n+1)(3n)(4π)(3n)[MMtot]2(n3)(ξ~2θ~)2(3n)}1/(n3)

 

=

(n+1)1(4π)(1)[MMtot]2ξ~4θ~n(n+1)(ξ~2θ~)2.

This means that, in equilibrium,

LHS

=

[n(n+1)]{(n+1)(4π)ξ~4θ~n(n+1)(ξ~2θ~)2}(ξ~3θ~')2(34π)2[θ~n+1ξ~2]0ξ~(σ2Gρc)θnξ4x2dξ

 

=

0ξ~(nσ24πGρc)θnξ4x2dξ.

In summary, then, we have,

0ξ~(nσ24πGρc)θnξ4x2dξ

=

3ξ~3θ~n+1xsurface2+0ξ~ξ2θn+1x2{[ξxdxdξ]2+(n3)[ξθdθdξ]}dξ.

Perhaps this looks better if the terms are rearranged to give,

3ξ~3θ~n+1xsurface2

=

0ξ~ξ2θn+1x2{(nσ24πGρc)ξ2θ[(dlnxdlnξ)2+(n3)(dlnθdlnξ)]}dξ.

Plug in Known Marginally Unstable Solution[edit]

As has been summarized in an accompanying discussion, we have found that, for marginally unstable pressure-truncated polytropic configurations, the eigenvector associated with the fundamental mode of radial oscillation is prescribed analytically by the following eigenfrequency-eigenfunction pair:

σc2=0

      and      

x=3(n1)2n[1+(n3n1)(1ξθn)dθdξ].

This means that,

[2n3(n1)]dxdξ

=

(n3n1)ddξ(θ'ξθn)

 

=

(n3n1)[θ'ξθnθ'ξ2θnn(θ')2ξθn+1]

 

=

(n3n1)[1ξθn(θn+2θ'ξ)θ'ξ2θnn(θ')2ξθn+1]

 

=

(3nn1)[1ξ+3θ'ξ2θn+n(θ')2ξθn+1].

Hence, also,

dlnxdlnξ=ξxdxdξ

=

(3nn1)[1+3θ'ξθn+n(θ')2θn+1][1+(n3n1)(θ'ξθn)]1

 

=

(3nn1)(n3n1)1[1+3θ'ξθn+n(θ')2θn+1][(n1n3)+(θ'ξθn)]1

 

=

[1+3θ'ξθn+n(θ')2θn+1][(n1n3)+(θ'ξθn)]1.

Rather, let's try:

ξ2x2[(dlnxdlnξ)2+(n3)(dlnθdlnξ)]

=

x2ξ2(ξxdxdξ)2+(n3)x2ξ2(ξθdθdξ)

 

=

ξ4{dxdξ}2+(n3)[ξ3θ'θ]x2

 

=

ξ4{3(n1)2n(3nn1)[1ξ+3θ'ξ2θn+n(θ')2ξθn+1]}2+(n3)[ξ3θ'θ]{3(n1)2n[1+(n3n1)(θ'ξθn)]}2

 

=

ξ2(n3)[32n]2{(n3)[1+3θ'ξθn+n(θ')2θn+1]2+ξ(θ'θ)[(n1)+(n3)(θ'ξθn)]2}

Hence, after setting σ2=0, the above rearranged integral relation becomes,

22n23(n3)[ξ~3θ~n+1xsurface2]

=

0ξ~ξ2θn+1{(n3)[1+3θ'ξθn+n(θ')2θn+1]2+ξ(θ'θ)[(n1)+(n3)(θ'ξθn)]2}dξ


Let's check to see whether the terms in this last expression balance out when we plug in the functions that are appropriate for the marginally unstable, n = 5 configuration, namely,

θ5=(3+ξ23)1/2,

     and    

dθ5dξ=ξ3(3+ξ23)3/2.

RHS Term 1

=

(n3)0ξ~ξ2θn+1[1+3θ'ξθn+n(θ')2θn+1]2dξ

 

=

20ξ~ξ2[(3+ξ23)1/2]6{1[ξ(3+ξ23)3/2]1ξ(3+ξ23)5/2+5[ξ232(3+ξ23)3][(3+ξ23)3]}2dξ

 

=

20ξ~33ξ2(3+ξ2)3{1(3+ξ23)+5ξ232}2dξ

 

=

2330ξ~ξ6dξ(3+ξ2)3

 

=

233[27ξ8(3+ξ2)9ξ4(3+ξ2)2+ξ(33/2523)tan1(ξ31/2)]03=233[352631/25π23].

RHS Term 2

=

0ξ~ξ3θnθ'[(n1)+(n3)(θ'ξθn)]2dξ

 

=

0ξ~ξ3(3+ξ23)5/2ξ3(3+ξ23)3/2{4213(3+ξ23)3/2(3+ξ23)5/2}2dξ

 

=

130ξ~(3ξ3+ξ2)4{423(3+ξ23)}2dξ

 

=

2330ξ~12(ξ3+ξ2)4{15ξ2}2dξ

 

=

233[123ξ8(3+ξ2)243ξ4(3+ξ2)2+162ξ2(3+ξ2)3+ξ2(33/2523)tan1(ξ31/2)]03

 

=

233525[2231/2π33]=233[3352531/25π23].

RHS Total

=

233[352633525]=3223[3225]=3223.

LHS

=

22n23(n3)[ξ~3θ~n+1xsurface2]

 

=

225223[33(33+32)32252]=233[(322)3]=3223.

Hence, the LHS = RHS.   Hooray!

See Also[edit]

 

A variational principle of great power is derived. It is naturally adapted for computers, and may be used to determine the stability of any fluid flow including those in differentially-rotating, self-gravitating stars and galaxies. The method also provides a powerful theoretical tool for studying general properties of eigenfunctions, and the relationships between secular and ordinary stability. In particular we prove the anti-sprial theorem indicating that no stable (or steady( mode can have a spiral structure.

  • B. F. Schutz, Jr. (1972), ApJSuppl., 24, 319: Linear Pulsations and Stability of Differentially Rotating Stellar Models. I. Newtonian Analysis
 

A systematic method is presented for deriving the Lagrangian governing the evolution of small perturbations of arbitrary flows of a self-gravitating perfect fluid. The method is applied to a differentially rotating stellar model; the result is a Lagrangian equivalent to that of D. Lynden-Bell & J. P. Ostriker (1967). A sufficient condition for stability of rotating stars, derived from this Lagrangian, is simplified greatly by using as trial functions not the three components of the Lagrangian displacement vector, but three scalar functions … This change of variables saves one from integrating twice over the star to find the effect of the perturbed gravitational field.

… we examine the special cases of (i) axially symmetric perturbations of a rotating star (as treated by S. Chandrasekhar & N. R. Lebovitz 1968); and (ii) perturbations of a nonrotating star (as treated by Chandrasekhar and Lebovitz 1964). We find that the stability criteria for those cases can also be simplified …

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