中国物理B ›› 2013, Vol. 22 ›› Issue (5): 59801-059801.doi: 10.1088/1674-1056/22/5/059801

• GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS • 上一篇    

Inflationary dynamics in the braneworld scenarios

张开源, 吴普训, 余洪伟   

  1. Center of Nonlinear Science and Department of Physics, Ningbo University, Ningbo 315211, China
  • 收稿日期:2012-09-08 修回日期:2012-10-14 出版日期:2013-04-01 发布日期:2013-04-01
  • 基金资助:
    Project supported by the National Natural Science Foundation of China (Grant Nos. 10935013, 11175093, 11222545, and 11075083), the Natural Science Foundation of Zhejiang Province of China (Grant Nos. Z6100077 and R6110518), the FANEDD (Grant No. 200922), the National Basic Research Program of China (Grant No. 2010CB832803), and K. C. Wong Magna Fund in Ningbo University of China.

Inflationary dynamics in the braneworld scenarios

Zhang Kai-Yuan (张开源), Wu Pu-Xun (吴普训), Yu Hong-Wei (余洪伟)   

  1. Center of Nonlinear Science and Department of Physics, Ningbo University, Ningbo 315211, China
  • Received:2012-09-08 Revised:2012-10-14 Online:2013-04-01 Published:2013-04-01
  • Contact: Wu Pu-Xun E-mail:wpx0227@gmail.com
  • Supported by:
    Project supported by the National Natural Science Foundation of China (Grant Nos. 10935013, 11175093, 11222545, and 11075083), the Natural Science Foundation of Zhejiang Province of China (Grant Nos. Z6100077 and R6110518), the FANEDD (Grant No. 200922), the National Basic Research Program of China (Grant No. 2010CB832803), and K. C. Wong Magna Fund in Ningbo University of China.

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摘要： We analyze the attractor behaviour of the inflation field in braneworld scenarios using the Hamilton-Jacobi formalism, where the Friedmann equation has the form of H2=ρ+ε√2ρ0ρ or H2=ρ+ερ2/2σ, with ε=±1. We find that in all models the linear homogeneous perturbation can decay exponentially as the scalar field rolls down its potential. However, in the case of a -ρ2 correction to the standard cosmology with ρ < σ, the existence of an attractor solution requires (σ-ρ)/φ2 > 1. Our results show that the perturbation decays more quickly in models with positive-energy correction than in the standard cosmology, which is opposite to the case of negative-energy correction. Thus, the positive-energy modification rather than the negative one can assist the inflation and widen the range of initial conditions.

关键词: inflation, braneworld, attractor

Abstract: We analyze the attractor behaviour of the inflation field in braneworld scenarios using the Hamilton-Jacobi formalism, where the Friedmann equation has the form of H2=ρ+ε√2ρ0ρ or H2=ρ+ερ2/2σ, with ε=±1. We find that in all models the linear homogeneous perturbation can decay exponentially as the scalar field rolls down its potential. However, in the case of a -ρ2 correction to the standard cosmology with ρ < σ, the existence of an attractor solution requires (σ-ρ)/φ2 > 1. Our results show that the perturbation decays more quickly in models with positive-energy correction than in the standard cosmology, which is opposite to the case of negative-energy correction. Thus, the positive-energy modification rather than the negative one can assist the inflation and widen the range of initial conditions.

Key words: inflation, braneworld, attractor

中图分类号:  (Cosmology)

  • 98.80.-k
04.50.-h (Higher-dimensional gravity and other theories of gravity)