Constraints on the chaotic inflationary scenario with a nonminimally coupled “inflaton” field from the cosmic microwave background radiation anisotropy

Eiichiro Komatsu; Toshifumi Futamase

doi:10.1103/PhysRevD.58.023004

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Constraints on the chaotic inflationary scenario with a nonminimally coupled “inflaton” field from the cosmic microwave background radiation anisotropy

Eiichiro Komatsu^* and Toshifumi Futamase^†

Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-77, Japan

^*E-mail address: komatsu@astr.tohoku.ac.jp
^†E-mail address: tof@astr.tohoku.ac.jp

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Phys. Rev. D 58, 023004 – Published 22 June, 1998Erratum Phys. Rev. D 58, 089902 (1998)

DOI: https://doi.org/10.1103/PhysRevD.58.023004

Abstract

We investigate the possibility to restrict the chaotic inflationary scenario with the large nonminimally coupled inflaton field $φ$ considered by Fakir and Unruh by means of the observed cosmic microwave background radiation (CMBR) anisotropy. This model is characterized by the condition $ξ > 1$ and $ψ \equiv 8 π G ξ φ^{2} ≫ 1$ where $ξ$ is the nonminimal coupling constant. We calculate the contributions of the long wavelength gravitational waves generated in the inflationary period to the CMBR anisotropy quadrupole moment. We obtain the constraint $λ / ξ^{2} = 1.8 \times 10^{- 8} / ψ_{i},$ where $λ$ is the self-coupling and $ψ_{i}$ means the initial value of $ψ .$ Combining this with the previously obtained constraint $\sqrt{λ / ξ^{2}} \approx (δ {T / T)}_{rms} = 1.1 \times 10^{- 5},$ we conclude that the initial value has to be $ψ_{i} \approx 1.6 \times 10^{3} .$ If the self-coupling has reasonable values of order $10^{- 2},$ then $ξ \approx 10^{4}$ and $φ_{i} \approx 10^{- 1} m_{Pl}$ where $m_{Pl}$ is the Planck mass.

Erratum

Erratum: Constraints on the chaotic inflationary scenario with a nonminimally coupled “inflaton” field from the cosmic microwave background radiation anisotropy [Phys. Rev. D 58, 023004 (1998)]

Eiichiro Komatsu and Toshifumi Futamase

Phys. Rev. D 58, 089902 (1998)

References (29)

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[c1] K. Sato, Mon. Not. R. Astron. Soc. 195, 467 (1981); Phys. Lett. 99B, 66 (1981).

[c2] A. Guth, Phys. Rev. D 23, 347 (1981).

[c3] A. D. Linde, Phys. Lett. 129B, 177 (1983).

[c4] R. Fakir and W. G. Unruh, Phys. Rev. D 41, 1783 (1990).

[c5] T. Futamase and K. Maeda, Phys. Rev. D 39, 399 (1989).

[c6] N. Makino and M. Sasaki, Prog. Theor. Phys. 86, 103 (1991).

[c7] R. Fakir, S. Habib, and W. G. Unruh, Astrophys. J. 394, 396 (1992).

[c8] D. S. Salopek, Phys. Rev. Lett. 69, 3602 (1992).

[c9] D. I. Kaiser, Phys. Rev. D 52, 4295 (1995).

[c10] R. K. Sachs and A. M. Wolfe, Astrophys. J. 147, 73 (1967).

[c11] L. F. Abbott and Mark B. Wise, Nucl. Phys. B244, 541 (1984).

[c12] M. Sasaki, Prog. Theor. Phys. 89, 1183 (1993).

[c13] C. W. Misner, K. S. Thorne, and J. A. Wheeler, Gravitation (Freeman, San Francisco, 1973).

[c14] S. Weinberg, Gravitation and Cosmology (Wiley, New York, 1972).

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[c16] John D. Barrow, José P. Mimoso, and Márcio R. de Garcia Maia, Phys. Rev. D 48, 3630 (1993).

[c17] L. F. Abbott and D. D. Harari, Nucl. Phys. B264, 487 (1986).

[c18] M. White, Phys. Rev. D 46, 4198 (1992).

[c19] L. Grishchuk and Y. Sidorov, Phys. Rev. D 42, 3413 (1990).

[c20] B. Allen and S. Koranda, Phys. Rev. D 50, 3713 (1994).

[c21] L. P. Grishchuk, Zh. Éksp. Teor. Fiz. 67, 825 (1974) [Sov. Phys. JETP 40, 409 (1975)]; Ann. (N.Y.) Acad. Sci. 302, 439 (1977).

[c22] N. D. Birrel and P. C. W. Davies, Quantum Fields in Curved Space (Cambridge University Press, Cambridge, England, 1982).

[c23] D. J. Fixsen et al., Astrophys. J. 473, 576 (1996).

[c24] C. L. Bennett et al., Astrophys. J. 464, L1 (1996).

[c25] L. M. Krauss and M. White, Phys. Rev. Lett. 69, 869 (1992).

[c26] V. F. Mukhanov, H. A. Feldman, and R. H. Brandenberger, Phys. Rep. 215, 203 (1992).

[c27] D. Hochberg and T. W. Kephart, Phys. Rev. D 51, 2687 (1995).

[c28] R. Fakir and W. G. Unruh, Phys. Rev. D 41, 1792 (1990).

[c29] F. S. Accetta, D. J. Zoller, and M. S. Turner, Phys. Rev. D 31, 3046 (1985).

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Constraints on the chaotic inflationary scenario with a nonminimally coupled “inflaton” field from the cosmic microwave background radiation anisotropy

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Erratum

Erratum: Constraints on the chaotic inflationary scenario with a nonminimally coupled “inflaton” field from the cosmic microwave background radiation anisotropy [Phys. Rev. D 58, 023004 (1998)]

References (29)

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