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Volumn 34, Issue 10, 1986, Pages 2934-2946

The R2 cosmology: Inflation without a phase transition

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EID: 17044379558     PISSN: 05562821     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevD.34.2934     Document Type: Article
Times cited : (305)

References (48)
  • 18
    • 84927187388 scopus 로고
    • It has been shown that initial anisotropies in a universe in which there is a massive scalar field will quickly decay away [, ]. This has been verified in, 143B, 83, where the wave function has been studied for an anisotropic universe. In the R2 model the scalar curvature R acts like a massive scalar field so that we can expect a similar decay of anisotropies., Phys. Lett.
    • (1980) J. B. Hartle and B. L. Hu, Phys. Rev. D , vol.21 , pp. 2756
    • Hawking, S.W.1    Luttrell, J.C.2
  • 29
    • 84927207536 scopus 로고    scopus 로고
    • Ya. B. Zeldovich and A. A. Starobinsky, Zh. Eksp. Teor. Fiz. 61, 2161, (1971)
  • 31
    • 84927207535 scopus 로고    scopus 로고
    • Pis'ma Zh. Eksp. Teor. Fiz. 26, 373 (1977)
  • 33
    • 84927207534 scopus 로고    scopus 로고
    • Strictly speaking we should use the renormalized energy-momentum tensor < Tμν > . Here, we assume that the vacuum polarization effect—that is, the difference between < Tηη > and peta given by Eq. (3.8)—will not change our present order-of-magnitude estimation. This assumption will be investigated in future work.


* 이 정보는 Elsevier사의 SCOPUS DB에서 KISTI가 분석하여 추출한 것입니다.