TY - JOUR

T1 - Cosmological evolution of general scalar fields in a brane-world cosmology

AU - Mizuno, Shuntaro

AU - Lee, Seung Joo

AU - Copeland, Edmund J.

PY - 2004/8

Y1 - 2004/8

N2 - We study the cosmology of a general scalar field and barotropic fluid during the early stage of a brane-world where the Friedmann constraint is dominated by the square of the energy density. Assuming both the scalar field and fluid are confined to the brane, we find a range of behavior depending on the form of the potential. Generalizing an approach developed for a standard Friedmann cosmology, in [A. de Ia Macorra and G. Piccinelli, Phys. Rev. D 61, 123503 (2000)], we show that the potential dependence V(φ) can be described through a parameter λ ≡- √2m5
3/2V'/ (√HV), where m5 is the five-dimensional Planck mass, H is the Hubble parameter, and V≡dV/dφ. For the case where λ asymptotes to zero, we show that the solution exhibits stable inflationary behavior. On the other hand if it approaches a finite constant, then V(φ)∞1/ φ2. For λ→∞ asymptotically, we find examples where it does so both with and without oscillating. In the latter case, the barOtropic fluid dominates the scalar field asymptotically. Finally we point out an interesting duality that leads to identical evolution equations in the high-energy ρ2 dominated regime and the low-energy p dominated regime..

AB - We study the cosmology of a general scalar field and barotropic fluid during the early stage of a brane-world where the Friedmann constraint is dominated by the square of the energy density. Assuming both the scalar field and fluid are confined to the brane, we find a range of behavior depending on the form of the potential. Generalizing an approach developed for a standard Friedmann cosmology, in [A. de Ia Macorra and G. Piccinelli, Phys. Rev. D 61, 123503 (2000)], we show that the potential dependence V(φ) can be described through a parameter λ ≡- √2m5
3/2V'/ (√HV), where m5 is the five-dimensional Planck mass, H is the Hubble parameter, and V≡dV/dφ. For the case where λ asymptotes to zero, we show that the solution exhibits stable inflationary behavior. On the other hand if it approaches a finite constant, then V(φ)∞1/ φ2. For λ→∞ asymptotically, we find examples where it does so both with and without oscillating. In the latter case, the barOtropic fluid dominates the scalar field asymptotically. Finally we point out an interesting duality that leads to identical evolution equations in the high-energy ρ2 dominated regime and the low-energy p dominated regime..

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U2 - 10.1103/PhysRevD.70.043525

DO - 10.1103/PhysRevD.70.043525

M3 - Article

AN - SCOPUS:37649031978

VL - 70

JO - Physical review D: Particles and fields

JF - Physical review D: Particles and fields

SN - 0556-2821

IS - 4 A

M1 - 43525

ER -