Enhanced inflation in the Dirac-Born-Infeld framework

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We consider the Einstein equations within the Dirac-Born-Infield (DBI) scenario for a spatially flat Friedmann-Robertson-Walker (FRW) spacetime without a cosmological constant. We derive the inflationary scenario by applying the symmetry transformations which preserve the form of the Friedmann and c...

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Autor principal: Chimento, L.P
Otros Autores: Lazkoz, R., Richarte, M.G
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2011
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Chimento, L.P. 
245 1 0 |a Enhanced inflation in the Dirac-Born-Infeld framework 
260 |c 2011 
270 1 0 |m Chimento, L.P.; Departamento de Física, Facultad de Ciencias Exactas y Naturales, Pabellón i, 1428 Buenos Aires, Argentina; email: chimento@df.uba.ar 
506 |2 openaire  |e Política editorial 
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520 3 |a We consider the Einstein equations within the Dirac-Born-Infield (DBI) scenario for a spatially flat Friedmann-Robertson-Walker (FRW) spacetime without a cosmological constant. We derive the inflationary scenario by applying the symmetry transformations which preserve the form of the Friedmann and conservation equations. These form invariance transformations generate a symmetry group parametrized by the Lorentz factor γ. We explicitly obtain an inflationary scenario by the cooperative effect of adding energy density into the Friedmann equation. For the case of a constant Lorentz factor, and under the slow roll assumption, we find the transformation rules for the scalar and tensor power spectra of perturbations as well as their ratio under the action of the form invariance symmetry group. Within this case and due to its relevance for the inflationary paradigm, we find the general solution of the dynamical equations for a DBI field driven by an exponential potential and show a broad set of inflationary solutions. The general solution can be split into three subsets and all these behave asymptotically as a power-law solution at early and at late times. © 2011 American Physical Society.  |l eng 
593 |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, Pabellón i, 1428 Buenos Aires, Argentina 
593 |a Fisika Teorikoa, Zientzia Eta Teknologia Fakultatea, Euskal Herriko Unibertsitatea, 644 Posta Kutxatila, 48080 Bilbao, Spain 
700 1 |a Lazkoz, R. 
700 1 |a Richarte, M.G. 
773 0 |d 2011  |g v. 83  |k n. 6  |p Phys Rev D Part Fields Gravit Cosmol  |x 15507998  |t Physical Review D - Particles, Fields, Gravitation and Cosmology 
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856 4 0 |u https://hdl.handle.net/20.500.12110/paper_15507998_v83_n6_p_Chimento  |y Handle 
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