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Exact Solutions and Scalar Fields in Gravity - Instituto Avanzado de ...

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98 EXACT SOLUTIONS AND SCALAR FIELDS IN GRAVITY<br />

The correspond<strong>in</strong>g scale factors are<br />

for <strong>and</strong><br />

for <strong>and</strong><br />

5. CONCLUSIONS<br />

For spaces, perfect fluid solutions imply that given <strong>and</strong><br />

the numerical value of is <strong>de</strong>term<strong>in</strong>ed by the amount of “matter”<br />

present while also its sign <strong>de</strong>pends on In other words, when space<br />

is non flat one can not freely choose the sign, or the <strong>de</strong>gree of coupl<strong>in</strong>g<br />

between the tensor <strong>and</strong> the scalar mo<strong>de</strong>s. Note the fact that <strong>in</strong> such<br />

spaces these fluids exp<strong>and</strong> <strong>in</strong> the same way, that is, expansion ignores the<br />

particular nature of “matter”. Even more disturb<strong>in</strong>g is the possibility<br />

that this evolution turns out to be the only k<strong>in</strong>d of expansion which<br />

can be given <strong>in</strong> terms of polynomial, transcen<strong>de</strong>ntal, or other fairly well<br />

known functions which may furthermore be also time <strong>in</strong>vertible. For<br />

the open space, a l<strong>in</strong>ear expansion is known to give a Milne<br />

Universe where space–time is, actually, flat M<strong>in</strong>kowski space. However,<br />

a l<strong>in</strong>ear expansion <strong>in</strong> is not a Milne solution.<br />

Acknowledgments<br />

This work was supported by CONACyT Grant No. 5–3672–E9312<br />

References<br />

[1] P.M. Garnavich et al., Astrophys. J. 509 (1998) 74; A G. Reiss et al., Astron. J.<br />

116 (1998) 1009; S. Perlmutter el al., Astrophys. J. 517 (1999) 565.<br />

[2] C. Brans <strong>and</strong> R. H. Dicke, Phys. Rev. 124 (1961) 925;<br />

[3] P. Chauvet, Astrophys. Space Sci. 90 (1983) 51.<br />

[4] P. Chauvet, <strong>and</strong> J.L. Cervantes-Cota, Phys. Rev. D52 (1995) 3416; P. Chauvet<br />

<strong>and</strong> O. Pimentel, Gen. Rel. Grav. 24 (1992) 243; P. Chauvet, J.L. Cervantes–<br />

Cota, <strong>and</strong> H.N. Núñez–Yépez, Class <strong>and</strong> Quantum Grav. 9 (1992) 1923.<br />

[5] P.G. Bergmann, Int. J. Theor. Phys. 1 (1968) 25; R.V. Wagoner, Phys. Rev. D<br />

1 (1970) 3209; K. Nordvedt, Astrophys. J. 161 (1970) 1059.<br />

[6] J.P. Mimoso <strong>and</strong> D. W<strong>and</strong>s, Phys. Rev. D51 (1995) 477; J.D. Barrow, Phys.<br />

Rev. D47, 5329 (1993); P. Chauvet <strong>and</strong> O. Obregón, Astrophys. Space Sci. 66

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