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Volumn 70, Issue 4, 2004, Pages 12-

Cosmology from a rolling massive scalar field on the anti-D3 brane of de Sitter vacua

Author keywords

[No Author keywords available]

Indexed keywords

ANISOTROPY; ARTICLE; COSMOS; DENSITY; ENERGY; MATHEMATICAL ANALYSIS;

EID: 45849154702     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.70.043536     Document Type: Article
Times cited : (78)

References (126)
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    • spatially homogeneous field configuration, a solution is characterized by initial position and velocity of the scalar field (Formula presented) We choose the origin of time when velocity of the scalar field is zero. Hence, the homogeneous solution is characterized by one parameter, the initial position of scalar field
    • In spatially homogeneous field configuration, a solution is characterized by initial position and velocity of the scalar field (Formula presented) We choose the origin of time when velocity of the scalar field is zero. Hence, the homogeneous solution is characterized by one parameter, the initial position of scalar field.
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    • R. Kallosh and A. Linde (private communication): Throughout the paper we have assumed that the volume of internal space is frozen as in KKLT model. When inflaton field is around zero, it was shown in 23 that the non-perturbative correction (17) to the tree level superpotential makes it possible to have a positive minimum at finite volume. This is in part due to the fact that the anti-D3 brane correction (19) is small. During the inflation the anti-D3 brane correction is again like (19) in which (Formula presented) should be replaced by (Formula presented) With this correction, however, one may not get anymore a local minimum for the supergravity potential during inflation in which φ is very large. In this case one may need to consider also α corrections to the Kahler potential 26 to study stabilization of the volume of internal space
    • R. Kallosh and A. Linde (private communication): Throughout the paper we have assumed that the volume of internal space is frozen as in KKLT model. When inflaton field is around zero, it was shown in 23 that the non-perturbative correction (17) to the tree level superpotential makes it possible to have a positive minimum at finite volume. This is in part due to the fact that the anti-D3 brane correction (19) is small. During the inflation the anti-D3 brane correction is again like (19) in which (Formula presented) should be replaced by (Formula presented) With this correction, however, one may not get anymore a local minimum for the supergravity potential during inflation in which φ is very large. In this case one may need to consider also α corrections to the Kahler potential 26 to study stabilization of the volume of internal space.
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    • Note that in some other cosmological models (Formula presented) can be negative. See, e.g., Ref. 33
    • Note that in some other cosmological models (Formula presented) can be negative. See, e.g., Ref. 33.
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* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.