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Title: Self-resonance after inflation: Oscillons, transients, and radiation domination

Abstract

Homogeneous oscillations of the inflaton after inflation can be unstable to small spatial perturbations even without coupling to other fields. We show that for inflaton potentials ∝Φ|2n near |Φ|=0 and flatter beyond some |Φ|=M, the inflaton condensate oscillations can lead to self-resonance, followed by its complete fragmentation. We find that for non-quadratic minima (n>1), shortly after backreaction, the equation of state parameter, w→1/3. If M << mPl, radiation domination is established within less than an e-fold of expansion after the end of inflation. In this case self-resonance is efficient and the condensate fragments into transient, localised spherical objects which are unstable and decay, leaving behind them a virialized field with mean kinetic and gradient energies much greater than the potential energy. This end-state yields w=1/3. When M~mPl we observe slow and steady, self-resonace that can last many e-folds before backreaction eventually shuts it off, followed by fragmentation and w→1/3. We provide analytical estimates for the duration to w→1/3 after inflation, which can be used as an upper bound (under certain assumptions) on the duration of the transition between the inflationary and the radiation dominated states of expansion. This upper bound can reduce uncertainties in CMB observables such as the spectralmore » tilt ns, and the tensor-to-scalar ratio r. For quadratic minima (n=1), w→0 regardless of the value of M. Finally, this is because when M << mPl, long-lived oscillons form within an e -fold after inflation, and collectively behave as pressureless dust thereafter. For M ~ m Pl , the self-resonance is inefficient and the condensate remains intact (ignoring long-term gravitational clustering) and keeps oscillating about the quadratic minimum, again implying w = 0 .« less

Authors:
 [1];  [2]
  1. Max Planck Inst. for Astrophysics, Garching (Germany); Univ. of Cambridge (United Kingdom)
  2. Rice Univ., Houston, TX (United States)
Publication Date:
Research Org.:
Rice Univ., Houston, TX (United States)
Sponsoring Org.:
USDOE Office of Science (SC)
OSTI Identifier:
1594798
Alternate Identifier(s):
OSTI ID: 1418396
Grant/Contract Number:  
SC0018216; PHY-106629
Resource Type:
Accepted Manuscript
Journal Name:
Physical Review D
Additional Journal Information:
Journal Volume: 97; Journal Issue: 2; Journal ID: ISSN 2470-0010
Publisher:
American Physical Society (APS)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Lozanov, Kaloian D., and Amin, Mustafa A. Self-resonance after inflation: Oscillons, transients, and radiation domination. United States: N. p., 2018. Web. doi:10.1103/PhysRevD.97.023533.
Lozanov, Kaloian D., & Amin, Mustafa A. Self-resonance after inflation: Oscillons, transients, and radiation domination. United States. doi:10.1103/PhysRevD.97.023533.
Lozanov, Kaloian D., and Amin, Mustafa A. Mon . "Self-resonance after inflation: Oscillons, transients, and radiation domination". United States. doi:10.1103/PhysRevD.97.023533. https://www.osti.gov/servlets/purl/1594798.
@article{osti_1594798,
title = {Self-resonance after inflation: Oscillons, transients, and radiation domination},
author = {Lozanov, Kaloian D. and Amin, Mustafa A.},
abstractNote = {Homogeneous oscillations of the inflaton after inflation can be unstable to small spatial perturbations even without coupling to other fields. We show that for inflaton potentials ∝Φ|2n near |Φ|=0 and flatter beyond some |Φ|=M, the inflaton condensate oscillations can lead to self-resonance, followed by its complete fragmentation. We find that for non-quadratic minima (n>1), shortly after backreaction, the equation of state parameter, w→1/3. If M << mPl, radiation domination is established within less than an e-fold of expansion after the end of inflation. In this case self-resonance is efficient and the condensate fragments into transient, localised spherical objects which are unstable and decay, leaving behind them a virialized field with mean kinetic and gradient energies much greater than the potential energy. This end-state yields w=1/3. When M~mPl we observe slow and steady, self-resonace that can last many e-folds before backreaction eventually shuts it off, followed by fragmentation and w→1/3. We provide analytical estimates for the duration to w→1/3 after inflation, which can be used as an upper bound (under certain assumptions) on the duration of the transition between the inflationary and the radiation dominated states of expansion. This upper bound can reduce uncertainties in CMB observables such as the spectral tilt ns, and the tensor-to-scalar ratio r. For quadratic minima (n=1), w→0 regardless of the value of M. Finally, this is because when M << mPl, long-lived oscillons form within an e -fold after inflation, and collectively behave as pressureless dust thereafter. For M ~ m Pl , the self-resonance is inefficient and the condensate remains intact (ignoring long-term gravitational clustering) and keeps oscillating about the quadratic minimum, again implying w = 0 .},
doi = {10.1103/PhysRevD.97.023533},
journal = {Physical Review D},
number = 2,
volume = 97,
place = {United States},
year = {2018},
month = {1}
}

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