Synergistic warm inflation

We consider an alternative warm inflationary scenario in which n scalar fields coupled to a dissipative matter fluid cooperate to produce power-law inflation. The scalar fields are driven by an exponential potential and the bulk dissipative pressure coefficient is linear in the expansion rate. We fi...

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Autor principal: Chimento, L.P
Otros Autores: Jakubi, A.S, Pavón, D., Zuccalá, N.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2002
Acceso en línea:Registro en Scopus
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100 1 |a Chimento, L.P. 
245 1 0 |a Synergistic warm inflation 
260 |c 2002 
506 |2 openaire  |e Política editorial 
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520 3 |a We consider an alternative warm inflationary scenario in which n scalar fields coupled to a dissipative matter fluid cooperate to produce power-law inflation. The scalar fields are driven by an exponential potential and the bulk dissipative pressure coefficient is linear in the expansion rate. We find that the entropy of the fluid attains its asymptotic value in a characteristic time proportional to the square of the number of fields. This scenario remains nearly isothermal along the inflationary stage. The perturbations in energy density and entropy are studied in the long-wavelength regime and seen to grow roughly as the square of the scale factor. They are shown to be compatible with COBE measurements of the fluctuations in temperature of the CMB.  |l eng 
593 |a Departamento de Física, Universidad de Buenos Aires, 1428 Buenos Aires, Argentina 
593 |a Departament de Física, Universidad Autónoma de Barcelona, 08193 Bellaterra, Spain 
690 1 0 |a ARTICLE 
690 1 0 |a CALCULATION 
690 1 0 |a DENSITY 
690 1 0 |a ENERGY 
690 1 0 |a ENTROPY 
690 1 0 |a PRESSURE 
690 1 0 |a SPECTRAL SENSITIVITY 
690 1 0 |a TEMPERATURE DEPENDENCE 
690 1 0 |a THERMAL ANALYSIS 
700 1 |a Jakubi, A.S. 
700 1 |a Pavón, D. 
700 1 |a Zuccalá, N. 
773 0 |d 2002  |g v. 65  |h pp. 835101-835109  |k n. 8A  |p Phys Rev D Part Fields Gravit Cosmol  |x 05562821  |w (AR-BaUEN)CENRE-394  |t Physical Review D - Particles, Fields, Gravitation and Cosmology 
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856 4 0 |u https://doi.org/10.1103/PhysRevD.65.083510  |y DOI 
856 4 0 |u https://hdl.handle.net/20.500.12110/paper_05562821_v65_n8A_p835101_Chimento  |y Handle 
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