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2024年10月30日
Chinese Physics C> 2018, Vol. 42> Issue(11) : 115102 DOI: 10.1088/1674-1137/42/11/115102

Asymptotic-de sitter inflation in the light of the planck data

  • 1.

      Department of physics, Rasht Branch, Islamic Azad University, Rasht, Iran

  • 2.

      Department of Physics, Ayatollah Amoli Branch, Islamic Azad University, Amol, Mazandaran, Iran

  • 3.

      Department of Physics, Qom Branch, Islamic Azad University, Qom, Iran

  • Planck 2015 data, emphasize that the background geometry during inflation is not pure de Sitter, but from the slow variation of Hubble parameter during the inflationary era, it can be quasi-de Sitter. This motivates us to consider an Asymptotic-de Sitter mode function for reconstructing of initial mode and primordial power spectrum of curvature perturbation. Using Markov Chain Monte Carlo (MCMC) method together with applying recent observational constraints from the Cosmic Microwave Background (CMB) data for the parameterized asymptotic initial mode in term of c, show some deviation from Bunch-Davies mode (c=1). Based on Planck 2015 data release the amplitude of scalar perturbations in 68% confidence level is 109 As=2.94-0.42+0.42 and deviation from Bunch-Davies mode is~0.05, i.e. c~1.05. In this parametrization, the CMB power spectrum of our model shows more red-tilt in comparison with ∧CDM model. Furthermore, we found upper limits for tensor-to-scaler ratio with different pivot scales.
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  • References

    [1] J. Martin and R. H. Brandenberger, Phys. Rev. D, 63:123501(2001)
    [2] V. M. Moukhanov, Physical Foundation Of Cosmology, (New York:Cambridge University Press, 2005)
    [3] S. Weinberg, Cosmology, (New York:Cambridge University Press, 2008)
    [4] A. H. Guth, Phys. Rev. D, 23:347(1981)
    [5] D. H. Lyth and A. R. Liddle, The primordial density perturbation:cosmology, inflation and the origin of structure, (New York:Cambridge University Press, 2009)
    [6] S. Dodelson, Modern Cosmology, (New York:Accademic press, 2003)
    [7] M. Bridges et al, Mon. Not. Roy. Astron. Soc., 381:68(2007)
    [8] Z. Guo et al, JCAP, 08:031(2011)
    [9] C. R. Contaldi et al, JCAP, 07:002(2003)
    [10] A. Iqbal, J. Prasad, T. Souradeep, and M. A. Malik, JCAP, 06:014(2015)
    [11] Y. Cai et al, Phys. Rev. D, 92:023518(2015)
    [12] B. A. Powell and W. H. Kinney, Phys. Rev. D, 76:063512(2007)
    [13] R. Emami, H. Firouzjahi, and M. Zarei, Phys. Rev. D, 90:023504(2014)
    [14] Y. Cai et al, JCAP, 08:020(2012)
    [15] Z. Liu et al, Phys. Rev. D, 88:063539(2013)
    [16] R. H. Brandenberger and J. Martin, arXiv:1211.6753
    [17] B. Greene et al, Extracting New Physics from the CMB, in the proceedings of 22nd Texas Symposium on Relativistic Astrophysics at Stanford University, Dec.13-17(2004) 0001
    [18] R. Kallosh and A. Linde, JCAP, 04:017(2007)
    [19] Y. Cai et al, Phys. Rev. D, 92:121303(2015)
    [20] T. S. Bunch and P. C. W. Davies, Proc. Roy. Soc. Lond. A, 360:117(1978)
    [21] R. Holman and A. J. Tolley, JCAP, 05:001(2008)
    [22] A. Ashoorioon and G. Shiu, JCAP, 03:025(2011)
    [23] S. Kundu, JCAP, 02:005(2012)
    [24] A. Ashoorioon et al, JCAP, 02:025(2014)
    [25] P. A. R. Ade et al, arXiv:1502.02114
    [26] M. Mohsenzadeh et al, Eur. Phys. J. C, 74:2920(2014)
    [27] E. Yusofi and M. Mohsenzadeh, JHEP, 09:020(2014) arXiv:1402.6968
    [28] E. Yusofi and M. Mohsenzadeh, Mod. Phys. Lett. A, 30:1550041(2015)
    [29] E. Yusofi and M. Mohsenzadeh, Phys. Lett. B, 735:261(2014)
    [30] M. Mohsenzadeh and E. Yusofi, Chinese Physics C, 41(8):085101(2017)
    [31] A. Sojasi et al, Chinese Physics C, 40(7):075101(2016)
    [32] E. Yusofi and M. Mohsenzadeh, DOI.10.1007/s10773-018-3689-3, arXiv:1506.02767
    [33] L. Bergstrom and U. H. Danielsson, JHEP, 0212:038(2002)
    [34] U. H. Danielsson, Phys. Rev. D, 66:023511(2002) hep-th/0203198
    [35] A. Lewis, A. Challinor, and A. Lasenby, Astrophys. J., 538:473(2000)
    [36] A. Lewis and S. Bridle, Phys. Rev. D, 66:103511(2002)
    [37] M. Trashorras, S. Nesseris, and J. Garcia-Bellido, Phys. Rev. D, 94:063511(2016)

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Ata Sojasi, Ebrahim Yusofi and Majid Mohsenzadeh. Asymptotic-de sitter inflation in the light of the planck data[J]. Chinese Physics C, 2018, 42(11): 115102. doi: 10.1088/1674-1137/42/11/115102
Ata Sojasi, Ebrahim Yusofi and Majid Mohsenzadeh. Asymptotic-de sitter inflation in the light of the planck data[J]. Chinese Physics C, 2018, 42(11): 115102.  doi: 10.1088/1674-1137/42/11/115102 shu
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Received: 2018-04-19
Revised: 2018-07-14
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    Supported by Islamic Azad University-Rasht Branch, Rasht, Iran

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Asymptotic-de sitter inflation in the light of the planck data

  • 1.  Department of physics, Rasht Branch, Islamic Azad University, Rasht, Iran
  • 2.  Department of Physics, Ayatollah Amoli Branch, Islamic Azad University, Amol, Mazandaran, Iran
  • 3.  Department of Physics, Qom Branch, Islamic Azad University, Qom, Iran
  • Received Date: 2018-04-19
  • Accepted Date: 2018-07-14
  • Available Online: 2018-11-05
Fund Project:  Supported by Islamic Azad University-Rasht Branch, Rasht, Iran

Abstract: Planck 2015 data, emphasize that the background geometry during inflation is not pure de Sitter, but from the slow variation of Hubble parameter during the inflationary era, it can be quasi-de Sitter. This motivates us to consider an Asymptotic-de Sitter mode function for reconstructing of initial mode and primordial power spectrum of curvature perturbation. Using Markov Chain Monte Carlo (MCMC) method together with applying recent observational constraints from the Cosmic Microwave Background (CMB) data for the parameterized asymptotic initial mode in term of c, show some deviation from Bunch-Davies mode (c=1). Based on Planck 2015 data release the amplitude of scalar perturbations in 68% confidence level is 109 As=2.94-0.42+0.42 and deviation from Bunch-Davies mode is~0.05, i.e. c~1.05. In this parametrization, the CMB power spectrum of our model shows more red-tilt in comparison with ∧CDM model. Furthermore, we found upper limits for tensor-to-scaler ratio with different pivot scales.

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