Gravitational waves from asymmetric oscillon dynamics?

Amin, Mustafa A.; Braden, Jonathan; Copeland, Edmund J.; Giblin, John T.; Solorio, Christian; Weiner, Zachary J.; Zhou, Shuang-Yong

doi:10.1103/physrevd.98.024040

Cited by 88 publications

(71 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…with 128 3 lattice points and throughout the time period considered in this Letter. We have noted the failure of a convergence test in our paper [1], and also a recent paper [2] has made this observation.…”

supporting

confidence: 63%

Erratum: Gravitational Waves from Oscillons after Inflation [Phys. Rev. Lett. 118 , 011303 (2017)]

Antusch¹,

Cefalà²,

Orani³

2018

Phys. Rev. Lett.

View full text Add to dashboard Cite

show abstract

supporting

confidence: 63%

Erratum: Gravitational Waves from Oscillons after Inflation [Phys. Rev. Lett. 118 , 011303 (2017)]

Antusch¹,

Cefalà²,

Orani³

2018

Phys. Rev. Lett.

View full text Add to dashboard Cite

show abstract

“…In the KKLT case the star mass is M P |W 0 | −1 V. We determined the field profile and the mass-radius behaviour for each case in the dilute regime. 36 A summary of the configurations obtained in this article can be seen in table 2 and a summary of expected mass ranges and radii for typically considered values of the overall volume and flux parameter are shown in figure 9. Similarly studying the formation of these objects we pointed out that the first condition listed at the beginning of section 4 (i.e.…”

Section: Discussionmentioning

confidence: 98%

“…the existence of a localized overdensity) is always satisfied independently of the initial conditions and of the details of the model. The enhancement of the density perturbations takes place if there 36 The relation of the mass of the object with the inverse mass of the corresponding particle is reminiscent of the fact that in gauge theories elementary particles have masses proportional to couplings and that of the solitonic objects to powers of the inverse couplings. This played a role in uncovering strong-weak dualities in field and string theories.…”

Section: Discussionmentioning

confidence: 99%

“…The absence of an analogous symmetry that stabilizes the localized configuration (see however [30]) makes oscillons long-lived but eventually they have to classically decay [31,32], radiating scalar waves to infinity. 3 Q-balls and oscillons have a rich phenomenology in terms of GW production [28,[34][35][36], baryogenesis [37][38][39][40], dark matter [41,42]. While Q-balls and oscillons can exist in the regime in which gravity is negligible, for other classes of compact objects gravity is the force that stabilizes the repulsive gradient pressure, while self-interactions can be absent.…”

Section: Jhep08(2018)070mentioning

confidence: 99%

See 1 more Smart Citation

Moduli stars

Krippendorf¹,

Muia

Quevedo

2018

J. High Energ. Phys.

View full text Add to dashboard Cite

We explore the possibility that (Bose-Einstein) condensation of scalar fields from string compactifications can lead to long-lived compact objects. Depending on the type of scalar fields we find different realisations of star-like and solitonic objects. We illustrate in the framework of type IIB string compactifications that closed string moduli can lead to heavy microscopic stars with masses of order V α M Planck , α = 1, 3/2, 5/3 where V is the volume of the extra dimensions. Macroscopic compact objects from ultra-light string axions are realised with masses of order e V 2/3 M Planck . Q-ball configurations can be obtained from open string moduli whereas the closed string sector gives rise to a new class of solutions, named PQ-balls, that arise in the two-field axion-modulus system. The stability, the potential for the formation, and the observability of moduli stars through gravitational waves are discussed. In particular we point out that during the early matter phase given by moduli domination, density perturbations grow by a factor V β with β > 2 and non-linear effects cannot be neglected.

show abstract

“…A lot of studies on gravitational waves emitted during the formation of oscillons can be found in the recent literature [29][30][31][32][33][34][35][36][37][38]. In this paper, we try to address the following question: How much do the properties of gravitational waves emitted from the formation of oscillons, such as the shape and the amplitude of the power spectrum, depend on the potential of a source scalar field.…”

Section: Jhep03(2021)021mentioning

confidence: 99%

Gravitational wave spectra from oscillon formation after inflation

Hiramatsu

Sfakianakis

Yamaguchi

2021

J. High Energ. Phys.

View full text Add to dashboard Cite

We systematically investigate the preheating behavior of single field inflation with an oscillon-supporting potential. We compute both the properties of the emitted gravitational waves as well as the number density and characteristics of the produced oscillons. By performing numerical simulations for a variety of potential types, we divide the analyzed potentials in two families, each of them containing potentials with varying large- or small-field dependence. We find that the shape of the spectrum and the amplitude of emitted gravitational waves have a universal feature with the peak around the physical wavenumber k/a ∼ m at the inflaton oscillation starting period, irrespective of the exact potential shape. This can be used as a smoking-gun for deducing the existence of a violent preheating phase and possible oscillon formation after inflation. Despite this apparent universality, we also find differences in the shape of the spectrum of emitted gravitational waves between the two families of potentials, leading to discriminating features between them. In particular, all potentials show the emergence of a two-peak structure in the gravitational wave spectrum, arising at the time of oscillon formation. However, potentials that exhibit efficient parametric resonance tend to smear out this structure and by the end of the simulation the two-peak structure is replaced by one broad peak in the GW spectrum. We further compute the number density and properties of the produced oscillons for each potential choice, finding differences in the number density and size distribution of stable oscillons and transient overdensities. We also perform a linear fluctuation analysis and use the corresponding Floquet charts to relate the results of our simulations to the structure of parametric resonance for the various potential types. We find that the growth rate of the scalar perturbations and the associated oscillon formation time are sensitive to the small-field shape of a potential while the macroscopic physical properties of oscillons such as the total number depend on the large-field shape of a potential.

show abstract

Gravitational waves from asymmetric oscillon dynamics?

Cited by 88 publications

References 37 publications

Erratum: Gravitational Waves from Oscillons after Inflation [Phys. Rev. Lett. 118 , 011303 (2017)]

Erratum: Gravitational Waves from Oscillons after Inflation [Phys. Rev. Lett. 118 , 011303 (2017)]

Moduli stars

Gravitational wave spectra from oscillon formation after inflation

Contact Info

Product

Resources

About