Logarithmic Duality of the Curvature Perturbation
Abstract: We study the comoving curvature perturbation $\mathcal{R}$ in the single-field inflation models whose potential can be approximated by a piecewise quadratic potential $V(\varphi)$ by using the $\delta N$ formalism. We find a general formula for $\mathcal{R}(\delta\varphi, \delta\pi)$, consisting of a sum of logarithmic functions of the field perturbation $\delta\varphi$ and the velocity perturbation $\delta\pi$ at the point of interest, as well as of $\delta\pi_*$ at the boundaries of each quadratic piece, which are functions of ($\delta\varphi, \delta\pi$) through the equation of motion. Each logarithmic expression has an equivalent dual expression, due to the second-order nature of the equation of motion for $\varphi$. We also clarify the condition under which $\mathcal{R}(\delta\varphi, \delta\pi)$ reduces to a single logarithm, which yields either the renowned ``exponential tail'' of the probability distribution function of $\mathcal{R}$ or a Gumbel-distribution-like tail.
- A. H. Guth, Phys. Rev. D23, 347 (1981).
- A. A. Starobinsky, Phys. Lett. 91B, 99 (1980), [Adv. Ser. Astrophys. Cosmol.3,130(1987)].
- V. F. Mukhanov and G. V. Chibisov, JETP Lett. 33, 532 (1981), [Pisma Zh. Eksp. Teor. Fiz.33,549(1981)].
- A. D. Linde, Phys. Lett. B 108, 389 (1982).
- A. Albrecht and P. J. Steinhardt, Phys. Rev. Lett. 48, 1220 (1982).
- V. F. Mukhanov, JETP Lett. 41, 493 (1985).
- M. Sasaki, Prog. Theor. Phys. 76, 1036 (1986).
- Y. Akrami et al. (Planck), Astron. Astrophys. 641, A10 (2020), arXiv:1807.06211 [astro-ph.CO] .
- T. M. C. Abbott et al. (DES), Phys. Rev. D 105, 023520 (2022), arXiv:2105.13549 [astro-ph.CO] .
- I. D. Zel’dovich, Ya.B.; Novikov, Soviet Astron. AJ (Engl. Transl. ), 10, 602 (1967).
- S. Hawking, Mon. Not. Roy. Astron. Soc. 152, 75 (1971).
- B. J. Carr and S. Hawking, Mon. Not. Roy. Astron. Soc. 168, 399 (1974).
- P. Meszaros, Astron. Astrophys. 37, 225 (1974).
- B. J. Carr, Astrophys. J. 201, 1 (1975).
- H. Noh and J.-c. Hwang, Phys. Rev. D 69, 104011 (2004).
- C. Carbone and S. Matarrese, Phys. Rev. D 71, 043508 (2005), arXiv:astro-ph/0407611 .
- K. Nakamura, Prog. Theor. Phys. 117, 17 (2007), arXiv:gr-qc/0605108 .
- M. Sasaki and E. D. Stewart, Prog. Theor. Phys. 95, 71 (1996), arXiv:astro-ph/9507001 .
- D. H. Lyth and Y. Rodriguez, Phys. Rev. Lett. 95, 121302 (2005), arXiv:astro-ph/0504045 .
- S. Young and C. T. Byrnes, JCAP 08, 052 (2013), arXiv:1307.4995 [astro-ph.CO] .
- V. Atal and C. Germani, Phys. Dark Univ. 24, 100275 (2019), arXiv:1811.07857 [astro-ph.CO] .
- R. Mahbub, Phys. Rev. D 102, 023538 (2020), arXiv:2005.03618 [astro-ph.CO] .
- S. Young, JCAP 05, 037 (2022), arXiv:2201.13345 [astro-ph.CO] .
- T. Matsubara and M. Sasaki, JCAP 10, 094 (2022), arXiv:2208.02941 [astro-ph.CO] .
- S. Pi and M. Sasaki, (2021), arXiv:2112.12680 [astro-ph.CO] .
- V. Vennin and A. A. Starobinsky, Eur. Phys. J. C 75, 413 (2015), arXiv:1506.04732 [hep-th] .
- V. Vennin, Stochastic inflation and primordial black holes, Ph.D. thesis, U. Paris-Saclay (2020), arXiv:2009.08715 [astro-ph.CO] .
- C. Animali and V. Vennin, (2022), arXiv:2210.03812 [astro-ph.CO] .
- We thank Jaume Garriga for pointing this out.
- In this figure, we only consider φ>0𝜑0\varphi>0italic_φ > 0. We will leave φ≤0𝜑0\varphi\leq 0italic_φ ≤ 0 case for future work.
- C. Unal, Phys. Rev. D 99, 041301 (2019), arXiv:1811.09151 [astro-ph.CO] .
- A. A. Starobinsky, Lect. Notes Phys. 246, 107 (1986).
- A. A. Starobinsky, Phys. Lett. B 117, 175 (1982).
- A. A. Starobinsky and J. Yokoyama, Phys. Rev. D 50, 6357 (1994), arXiv:astro-ph/9407016 .
Paper Prompts
Sign up for free to create and run prompts on this paper using GPT-5.
Top Community Prompts
Collections
Sign up for free to add this paper to one or more collections.