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1978 Collas Tests.Pdf LETTERE AL NUOVO C~MENTO VOL. 21, N. 2 14 Gennaio 1978 Simple Tests for Proposed Interior Kerr Metrics. P. COLLAS Department o] Physics and Astronomy Cali]ornia State University - Northridge, Cal. 91330 (rieevuto il 24 Agosto t977; manoscritto revisionato ricevuto il 21 Novembre 1977) An extremely important problem in astrophysics is that of obtaining a metric for the interior of a rotating body. This is, for example, necessary for the description of the gravitational field (along with pressure and energy density ) inside a rotating star. A special case of interest is to seek a physical, stationary and axissymmetric solution which can be matched--more or less smoothly (~)--to the Kerr (exterior) solution and which describes a rotating per]eel or nonper]ect (anisotropic pressure) fluid. Although straightforward in principle, the problem is very difficult (2). HERNANDEZ (i) outlined a method for constructing exact interior solution which might serve as sources for the Kerr metric; he later (3) reformulated his method making use of Boyer-Lindquist co-ordinates (4) and proposed a solution. Briefly, the Hernandez method consists of guessing certain arbitrary functions which appear in a generaliza- tion of the Kerr metric; the guessed metric matches the Kerr metric on a suitable surface (5) and, in the limit of no rotation, goes into the interior Schwarzschi]d solution. Other generalizations of the Kerr metric which do not have the interior Schwarzschild as a limiting case may, of course, be written and examined (5.~). Ultimately, one must calculate the physical components of the stress-energy tensor in a locally nonrotating frame (LNRF) (7) to find out whether one is dealing with a physically meaningful fluid. This calculation is very tedious even with the aid of a computer. In this note we wish to point out simple tests which enable one to investigate and if necessary discard bad metrics without any loss of time. This method consists of (~) For the precise conditions, see, ~V. C. ]-IER,N'ANDEZ jr.: Phys. Rev., 159, 1070 (1967). (~) J. B, HARTLE: Aslrophys. Journ., 150, 1005 (1967) gives the components of the Ricci tensor in his appendix. (a) W. C. HERNANDEZ ir.: Phys. Rev., 167, 1180 (1968). (4) t~. H. ]3OYER and R. LINDQUIST: Journ. 3lath. Phys., 8, 265 (1967). (a) A. KR~,SINSKI: Institute of Astronomy, Polish Academy of Sciences preprint No. 63, W'arsaw (May 1976), has shown that the surface of a source of the Kerr metric should be given by r = eonst ill Boyer=Liquist co-ordinates. (0) P. COI,LAS and J. K. LAWRENCE: General Relativity and Gravitation, 7, 715 (1976). (7) J. ~V~. BARDEEN: Astrophys. Journ., 162, 71 (1970), sect. 6, and appendices A, B, and C ; J.M. BARDEEN and R. V. ~VAGONER: Astrophys. Journ., 167, 359 (1971), sect. 2 and 9; J. M. BARDEEX, ~vV. H. PRESS and S. A_, TEUKOLSKu Astrophys. Journ., 17g, 347 (1972), sect, 3. 68 SIMPLE TESTS FOR PROPOSED INTERIOR KERR METRICS 69 examining %he behavior of the red-shift observed at infinity for photons emitted in an LNRF as this frame approaches the center of symmetry from different directions. LNRF are defined so as to cancel out, as much as possible, the frame-dragging effects due to mass' rotation, and consequently physical processes analysed in such frames appear far simpler than in other kinds of co-ordinate frames. As can be seen in the examples below singularities, event horizons, and other anomalies show up readily. Consider the stationary and axissymmetric line element (1) ds 2 = -- exp [2v] dt 2 + exp [2~p](d(p -- o9 dt)`' + exp [2/t`'] dr" + exp [2tt3] dO:, where the five metric functions v, % ~, #~ and #~ depend only on r and 0. In addition, the metric is assumed to be asymptotically fiat; thus at spatial infinity v, r and it: must vanish. It is easy to show (~) that the red-shift observed at infinity for photons emitted in an LNRF at (r, 0) is given by (2) z= exp [--v] (1 -- a)L~-- 1 , where L is the photon's component of angular momentum parallel to the symmetry axis and E is the photon's energy (both conserved a long null geodesics ) (s). Further- more, (o is the angular velocity of the LNRF as seen from infinity, while v can be con- sidered the generM-relativistic gravitational potential (~). Example I. The Kerr metric. - Let us consider the well-known ease of the Kerr metric in Boyer-Lindquist (4) co-ordinates A -- a`' sin a 0 @`' B sin ~- 0 4amr sin e 0 ._ @`' d~v: d~v dt, (3) ds: @2 dt`' + ~ dr 2 + @2 dO 2 § @2 where f ~ = r 2 ~-- 2mr 4- a 2 , (4) @2 = r2_~ a 2cOs ~0, B = 0 `2 + a2):--a~A sin20 . In this case eq. (2) for the red-shift is (5) When a2<m 2 the larger of the roots of A=O, r+=m-~ (m`'--a2) 89 is an event horizon (z-> oo). The vanishing of @`' for 0 = zt/2, r= 0, gives us the ring singula-, rity (4). The function B is positive in the physical range of the variables except at 0 = ~t/2, r = 0, where it vanishes linearly, and therefore it does not affect z. Tile sta- tionary limit surface does not appear in eq. (5) since it is not an event horizon for our photons. (8) Note that since tlle energy of a physical particle must always be positive as measured by the LNRF observer, we must require E--o)L > 0; for the origin of this condition see the second of ref. (7). 70 P. COLLAS When a ~ > m s, A ~ 0 in the physical range of the variables, and so there is no event horizon. We have a naked singularity, and the red-shift at r ~ 0 is discontinuous with respect to the angle; e.g., for L = 0 photons z 0=g/s--> c~ , Z 0#~/s = 0 . ',r=O Ir=O Example II. Hogan's metric. - HOGAN (9) proposed an interior Kerr solution which, in Boyer-Lindquist co-ordinates, is given by (6) ds2= --dr2+ (1 --/)(dt -k asinS 0d~0) 2 -k (rS+ aS) sinS0d~2 + (02/Z) drS + 02d02 , where 0 ~ is given by eq. (4), Z = rS--q R2 0eq - a 2 , ] = (~%/1--qb~-- 89 R = oS/r, b is ~ constant, q = 2m/b 3 and b > 2m. Line element (6) matches continuously to (3) on the closed 2-surface ~=71+ V1 bz ], where (b/2) 2 > m s>a s . Moreover for a = 0 it becomes the interior Schwarzschild solution for ~ homogeneous sphere of perfect fluid of radius b. Unfortunately it is easy to see that line element (6) becomes complex in the physical range of the variables. The function ] can be rewritten as follows: F 1 I qm m(r ~ ~- a s cos s 0) s _3~(l_~)(12m(rS~aSc~ (7) ] = -~ [5- b bar s b3rs ]j The term --2ma 4cos 40/(bar 2) in the square root will grow, for 0 ~ ~/2, as r-> 0 and f will become complex. The red-shift (we consider/5 = 0 photons for simplicity) is given by z= [rS@aS~-(1--])aSsinsO] 89 1 0 s ] + a 2 sin s 0 and, likewise, becomes complex (it is interesting that for 0 = ~/2, z is well-behaved all the way to r 0). Example III. Another interior Kerr metric. Consider the line element (again in Boyer-Lindquist co-ordinates) (8) ds 2 -- A~ -- a2 sin20 dt-" -k 02 dr s q- 02 d02 q- B--- sin 20 d~v2 4a]o sin 20 d~0 dt, 02 ~ 02 0 s (~) P. A. HO(~A.X: Lett. Nuovo Cimento, 16, 33 (1976). SIMPLE TESTS FOR PROPOSED II~T:ERIOR KERR METRICS 71 where ~ is given by eq. (4), and A i = r2 -~- a2 -- 2]i, i~0,1, B = (r 2 + a2)2--a2Aosin~O, (9) 1 .....ro1 ro ' mr 4 /1- r~" We require that r o > qm/4. Line element (8) is a slight generalization of the line alement investigated by LAWREt~CE and the author (~); it matches continuously the Kerr metric (3) on the ellipsoid r: % (5) since /i(ro) = mro, i= 0, 1 and ]-]0 =m dT r=ro (in fact it satisfies Hernandez' continuity conditions (1)). Furthermore line element (8) for a = 0 becomes ~he interior Schwarzschild solution for a sphere of radius r o. The red-shift (again L = 0 for simplicity) is now given by (10) z= V ~oB 1. In this case A o > 0, and B~> 0 in the physical range of the variables; B vanishes only at 0 = z/2, r = 0, where, now, it vanishes quadratically and again it does not affect z. Therefore there is no event horizon. The ring singularity at ~2= 0 is still there, unfortunately, and gives rise to finite red-shift at r ~ 0, but discontinuous in 0: / (11) z o~nt2 = 0 , z o=nt2 = V1 + 2~z-- 1 , r=o Jr=o where ( / 4 7o 1+ r ro ] One may, of course, choose a different ]0; for example in ]o with the property ]o = O(re) as r~0, c>2, would make z=0 at r=0 and continuous. However, that does not eliminate the trouble. This is because z(r, O) for any given r, 0 must either depend on the parameter a, or, otherwise, be equal to the nonrotating limit z at that point. For the present case the nonrotating limit is the interior Schwarzschild metric, and we 72 P. COLLAB obtain zl~=o = 1, 3 1------1 ro which is positive definite (and becomes infinite for r o = qm/4 as expected).
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