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Oscillons After Inflation
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Oscillons are massive, long-lived, localized excitations of a scalar field. We show that in a large class of well-motivated single-field models, inflation is followed by self-resonance, leading to copious oscillon generation and a lengthy period of oscillon domination. These models are characterized by an inflaton potential which has a quadratic minimum and is shallower than quadratic away from the minimum. This set includes both string monodromy models and a class of supergravity inspired scenarios, and is in good agreement with the current central values of the concordance cosmology parameters. We assume that the inflaton is weakly coupled to other fields, so as not to quickly drain energy from the oscillons or prevent them from forming. An oscillon-dominated universe has a greatly enhanced primordial power spectrum on very small scales relative to that seen with a quadratic potential, possibly leading to novel gravitational effects in the early universe.
Forward citations
Cited by 11 Pith papers
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Oscillon Formation in Palatini Modified Gravity Theories
Oscillons form in Palatini modified gravity with non-minimal coupling during preheating, yielding extended oscillon domination and ultra-high-frequency gravitational waves in the range of planned detectors.
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Unified theory of oscillons and modes
Oscillons are reinterpreted as localized resonant modes from threshold or antibound modes via nonlinearity, with wobblerons as new kink-oscillon bound states.
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Multi-field oscillons/I-balls in the Friedberg-Lee-Sirlin model
Multi-field oscillons in the Friedberg-Lee-Sirlin model form bound states of two co-located oscillons that oscillate at their respective masses due to attractive interactions.
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Preheating and oscillon formation in Einstein-scalar-Gauss-Bonnet gravity
Simulations in Einstein-scalar-Gauss-Bonnet gravity show oscillons form with similar properties to standard cases but trigger EFT breakdown for large couplings via high local curvatures.
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Late-Time Oscillating Quintessence in Light of DESI
A late-onset oscillating quintessence model improves the fit to DESI plus supernova and CMB data by Delta chi squared of about 9 over Lambda CDM, driven by background expansion.
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Oscillon Formation in Palatini Modified Gravity Theories
Numerical simulations show oscillons form and dominate for an extended period in Palatini gravity with non-minimal coupling, producing ultra-high-frequency gravitational waves potentially accessible to future detectors.
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Self-resonance preheating in deformed attractor models: oscillon formation and evolution
Deformed alpha-attractor T-models with a Gaussian feature near the minimum yield more smaller shorter-lived oscillons during self-resonance preheating, suppressing energy in oscillons and altering the high-frequency g...
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Equation of state during (p)reheating with trilinear interactions
Lattice simulations show that the post-inflationary equation of state with trilinear interactions returns to zero after an initial deviation, substantially lowering stochastic gravitational wave amplitudes relative to...
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From WIMP to FIMP during reheating: collider vs non-collider probes for p-wave annihilation
Collider experiments can strongly constrain p-wave-suppressed derivative operators and thereby limit reheating temperature, DM mass, and interaction scale needed to match observed DM abundance during reheating.
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ACT DR6+Planck impact on inflation with non-zero vacuum expectation value and the post-inflationary behavior
Updated constraints on non-zero VEV parameter M from ACT+Planck data, plus lattice simulations showing oscillon formation and reheating implications.
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Lectures on Reheating after Inflation
Lecture notes providing a generic introduction to reheating after inflation, covering its theoretical, phenomenological, and observational aspects.
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