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On the uniqueness of the equilibrium configurations of slowy rotating relativistic fluids
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14.This implies that on the star boundary a fact which simplifies some arguments. Equations of state of the form for can be allowed provided ρ(p) is more differentiable. See J. R. Savage, Ph. D. thesis, University of Alberta, 1980.
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21.More precisely we should formulate these conditions also in terms of Cantor's weighted Sobolev spaces as in Sec. 4. The result then follows from Ref. 5.
22.The modified potential U has continuous derivatives across the star boundary which is necessary to have a ‐action of the diffeomorphism group on P. Since U and determine each other for given constant a we will continue to calculate with U but remember that the manifold structure is defined in terms of See Ref. 2 for more details on this point.
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25.Equations (4.9) of Ref. 2 on the spherical background.
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27.In this formalism the central value of U is kept fixed. But this is all right since it is already known at this point that
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