Exact Bianchi type I models for an exponential-potential scalar field

A non-local transformation is used to linearize the evolution equation for Bianchi type I universes filled with an exponential-potential scalar field. Among the many new explicit solutions there is a family which shows, for different parameter ranges, the two generic asymptotic behaviours that were...

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Autor principal: Aguirregabiria, J.M
Otros Autores: Chimento, L.P
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 1996
Acceso en línea:Registro en Scopus
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Registro en la Biblioteca Digital
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245 1 0 |a Exact Bianchi type I models for an exponential-potential scalar field 
260 |c 1996 
270 1 0 |m Aguirregabiria, J.M.; Física Teórica, Universidad del País Vasco, Apdo. 644, 48080 Bilbao, Spain 
506 |2 openaire  |e Política editorial 
504 |a Aguirregabiria, J.M., Feinstein, A., Ibañez, J., (1993) Phys. Rev. D, 48, p. 4662 
504 |a Salam, A., Sezgin, E., (1984) Phys. Lett., 147 B, p. 47 
504 |a Fradkin, E.S., Tseytlin, A.A., (1985) Phys. Lett., 158 B, p. 316 
504 |a Campell, B.A., Linde, A., Olive, K.A., (1991) Nucl. Phys. B, 355, p. 146 
504 |a Ozer, M., Taha, M.O., (1992) Phys. Rev. D, 45, p. 997 
504 |a Easther, R., (1993) Class. Quantum Grav., 10, p. 2203 
504 |a Burd, A.B., Barro, J.D., (1988) Nucl. Phys. B, 308, p. 929 
504 |a Salopek, D.S., Bond, J.R., (1990) Phys. Rev. D, 42, p. 3936 
504 |a Ratra, B., (1992) Phys. Rev. D, 45, p. 1913 
504 |a Chimento, L.P., (1996) Form Invariance of Differential Equations in General Relativity, , submitted 
504 |a Lidsey, J.E., (1992) Class. Quantum Grav., 9, p. 1239 
504 |a Alé, M.G., Chimento, L.P., (1995) Class. Quantum Grav., 12, p. 101 
520 3 |a A non-local transformation is used to linearize the evolution equation for Bianchi type I universes filled with an exponential-potential scalar field. Among the many new explicit solutions there is a family which shows, for different parameter ranges, the two generic asymptotic behaviours that were previously found in numerical and qualitative analyses. A simpler expression for the general solution allows a better insight into the problem and reveals a damped oscillatory behaviour which corresponds to an effective negative cosmological constant. We are also now able to discuss the existence of initial and final singularities. We found families of explicit singular solutions which represent universes which after evolving from a singularity reach a final anisotropic or isotropic Friedmann-Robertson-Walker stage. There are also solutions which avoid the initial singularity and others with a finite time span. © 1996 IOP Publishing Ltd.  |l eng 
593 |a Física Teórica, Universidad del País Vasco, Apdo. 644, 48080 Bilbao, Spain 
593 |a Departamento de Física, Universidad de Buenos Aires, Ciudad Universitaria, 1428 Buenos Aires, Argentina 
700 1 |a Chimento, L.P. 
773 0 |d 1996  |g v. 13  |h pp. 3197-3209  |k n. 12  |p Classical Quantum Gravity  |x 02649381  |w (AR-BaUEN)CENRE-326  |t Classical and Quantum Gravity 
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