\begin{document}$ R^2 $\end{document}-corrected dark energy (DE) models in \begin{document}$ F(R) $\end{document} gravity have been widely investigated in recent years, which not only removes the weak singularity potentially present in DE models but also provide us with a unified picture of the cosmic history, including the inflationary and DE epochs. Towards the unified interpretation of dynamical DE all over the cosmic history in the class of \begin{document}$ R^2 $\end{document}-corrected DE models, we explore the universal features of the scalaron dynamics in the radiation-dominated epoch, along with the chameleon mechanism, by keeping our eyes on the inflationary and DE epochs. We show that the scalaron evolution does not follow a surfing solution and is mostly adiabatic before big bang nucleosynthesis (BBN), even properly including the kick by the nonperturbative QCD phase transition, hence a catastrophic consequence claimed in the literature is not applied to this class of DE models. This is due to the presence of the gigantic scale hierarchy between \begin{document}$ R^2 $\end{document} correction and DE, so is the universal feature for the class of \begin{document}$ R^2 $\end{document}-corrected DE models. The prospects for the post- or onset-inflationary epoch would be pretty different from what the standard \begin{document}$ R^2 $\end{document} inflationary scenario undergoes due to the presence of the chameleon mechanism."> Towards a unified interpretation of the early Universe in <i>R</i><sup>2</sup>-corrected dark energy model of <i>F</i>(<i>R</i>) gravity -
  • [1]

    Y. Akramiet al. (Planck), Astron. Astrophys. A10, 641 (2020), arXiv:1807.06211[astroph.CO

  • [2]

    J. Martin, Astrophys. Space Sci. Proc.45, 41 (2016), arXiv:1502.05733[astro-ph.CO

  • [3]

    A. G. Riesset al. (Supernova Search Team), Astron. J.116, 1009 (1998), arXiv:astroph/9805201

  • [4]

    S. Perlmutteret al. (Supernova Cosmology Project), Astrophys. J.517, 565 (1999), arXiv:astro-ph/9812133

  • [5]

    P. A. Zylaet al. (Particle Data Group), PTEP2020, 083C (2020)

  • [6]

    S. Nojiri, S. D. Odintsov, and V. K. Oikonomou, Phys. Rept.692, 1 (2017), arXiv:1705.11098[gr-qc

  • [7]

    L. Heisenberg, Phys. Rept.796, 1 (2019), arXiv:1807.01725[gr-qc

  • [8]

    A. De Felice and S. Tsujikawa, Living Rev. Rel.13, 3 (2010), arXiv:1002.4928[gr-qc

  • [9]

    S. A. Appleby and R. A. Battye, JCAP05, 019 (2008), arXiv:0803.1081[astro-ph

  • [10]

    A. V. Frolov, Phys. Rev. Lett.101, 061103 (2008), arXiv:0803.2500[astro-ph

  • [11]

    A. Dev, D. Jain, S. Jhinganet al., Phys. Rev. D78, 083515 (2008), arXiv: 0807.3445[hep-th]

  • [12]

    T. Kobayashi and K.-i. Maeda, Phys. Rev. D79, 024009 (2009), arXiv:0810.5664[astro-ph

  • [13]

    S. A. Appleby, R. A. Battye, and A. A. Starobinsky, JCAP06, 005 (2010), arXiv:0909.1737[astro-ph.CO

  • [14]

    C.-C. Lee, C.-Q. Geng, and L. Yang, Prog. Theor. Phys.128, 415 (2012), arXiv:1201.4546[astro-ph.CO

  • [15]

    A. A. Starobinsky, Phys. Lett. B91, 99 (1980)

  • [16]

    S. D. Odintsov and V. K. Oikonomou, Class. Quant. Grav.33, 125029 (2016), arXiv:1602.03309[gr-qc

  • [17]

    S. D. Odintsov, V. K. Oikonomou, and L. Sebastiani, Nucl. Phys. B923, 608 (2017), arXiv:1708.08346[gr-qc

  • [18]

    S. Nojiri, S. D. Odintsov, and V. K. Oikonomou, Phys. Dark Univ.29, 100602 (2020), arXiv:1912.13128[gr-qc

  • [19]

    V. K. Oikonomou, Phys. Rev. D103, 044036 (2021), arXiv:2012.00586[astro-ph.CO

  • [20]

    S. D. Odintsov and V. K. Oikonomou, Phys. Rev. D99, 104070 (2019), arXiv:1905.03496[gr-qc

  • [21]

    S. D. Odintsov and V. K. Oikonomou, Phys. Rev. D101, 044009 (2020), arXiv:2001.06830[gr-qc

  • [22]

    S. D. Odintsov and V. K. Oikonomou, Phys. Rev. D104, 124065 (2021), arXiv:2112.06269[gr-qc

  • [23]

    V. K. Oikonomou and I. Giannakoudi, (2022), arXiv: 2205.08599[gr-qc]

  • [24]

    M. Artymowski and Z. Lalak, JCAP09, 036 (2014), arXiv:1405.7818[hep-th

  • [25]

    C.-Q. Geng, C.-C. Lee, and S. Lin, Astrophys. Space Sci.360, 21 (2015), arXiv:1506.03253[astro-ph.CO

  • [26]

    M. Yashiki, N. Sakai, and R. Saito, Phys. Rev. D102, 043504 (2020), arXiv:2004.00864[astro-ph.CO

  • [27]

    V. K. Oikonomou, Phys. Rev. D103, 124028 (2021), arXiv:2012.01312[gr-qc

  • [28]

    V. K. Oikonomou and I. Giannakoudi, Nucl. Phys. B978, 115779 (2022), arXiv:2204.02454[gr-qc

  • [29]

    A. L. Erickcek, N. Barnaby, C. Burrageet al., Phys. Rev. Lett.110, 171101 (2013), arXiv:1304.0009[astro-ph.CO

  • [30]

    A. L. Erickcek, N. Barnaby, C. Burrageet al., Phys. Rev. D89, 084074 (2014), arXiv:1310.5149[astro-ph.CO

  • [31]

    G. S. Bali, F. Bruckmann, G. Endrödiet al., JHEP08, 177 (2014), arXiv:1406.0269[hep-lat

  • [32]

    T. Katsuragawa, T. Nakamura, T. Ikedaet al., Phys. Rev. D99, 124050 (2019), arXiv:1902.02494[gr-qc

  • [33]

    J. A. R. Cembranos, Phys. Rev. Lett.102, 141301 (2009), arXiv:0809.1653[hep-ph

  • [34]

    L. Husdal, Galaxies4, 78 (2016), arXiv:1609.04979[astro-ph.CO

  • [35]

    H. Chen, T. Katsuragawa, S. Matsuzakiet al., JHEP02, 155 (2020), arXiv:1908.04146[hep-ph

  • [36]

    H. Motohashi and A. Nishizawa, Phys. Rev. D86, 083514 (2012), arXiv:1204.1472[astroph.CO

  • [37]

    A. Nishizawa and H. Motohashi, Phys. Rev. D89, 063541 (2014), arXiv:1401.1023[astroph.CO

  • [38]

    A. D. Dolgov and D. P. Kirilova, Sov. J. Nucl. Phys.51, 172 (1990)

  • [39]

    J. H. Traschen and R. H. Brandenberger, Phys. Rev. D42, 2491 (1990)

  • [40]

    L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. Lett.73, 3195 (1994), arXiv:hepth/9405187

  • [41]

    Y. Shtanov, J. H. Traschen, and R. H. Brandenberger, Phys. Rev. D51, 5438 (1995), arXiv:hep-ph/9407247

  • [42]

    L. Kofman, A. D. Linde, and A. A. Starobinsky, Phys. Rev. D56, 3258 (1997), arXiv:hepph/9704452

  • [43]

    M. A. Amin, M. P. Hertzberg, D. I. Kaiseret al., Int. J. Mod. Phys. D24, 1530003 (2014), arXiv:1410.3808[hep-ph

  • [44]

    K. D. Lozanov, (2019), arXiv: 1907.04402[astro-ph.CO]

  • [45]

    A. Berera, Phys. Rev. Lett.75, 3218 (1995), arXiv:astro-ph/9509049

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