Scalar induced gravitational waves in inflation with gravitationally enhanced friction

Fu, Chengjie; Wu, Puxun; Yu, Hongwei

doi:10.1103/physrevd.101.023529

Cited by 81 publications

(66 citation statements)

References 57 publications

(81 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Recent studies confirm that the energy density can be parameterized as GW ( f ) ∼ f n [72,109,110]. In this regard, for the case A H we estimate GW ∼ f 1.78 for f < f c = 3.54 × 10 −3 Hz, and GW ∼ f −2.69 for f > f c .…”

Section: Induced Gravitational Wavessupporting

confidence: 55%

Primordial black holes formation in the inflationary model with field-dependent kinetic term for quartic and natural potentials

Solbi

Karami

2021

Eur. Phys. J. C

View full text Add to dashboard Cite

Within the framework of inflationary model with field-dependent kinetic term for quartic and natural potentials, we investigate generation of the primordial black holes (PBHs) and induced gravitational waves (GWs). In this setup, we consider a kinetic function as $$G(\phi )=g_I(\phi )\big (1+g_{II}(\phi )\big )$$ G ( ϕ ) = g I ( ϕ ) ( 1 + g II ( ϕ ) ) and show that in the presence of first term $$g_I(\phi )$$ g I ( ϕ ) both quartic and natural potentials, in contrast to the standard model of inflation, can be consistent, with the 68% CL of Planck observations. Besides, the second term $$g_{II}(\phi )$$ g II ( ϕ ) can cause a significant enhancement in the primordial curvature perturbations at the small scales which results the PBHs formation. For the both potentials, we obtain an enhancement in the scalar power spectrum at the scales $$k\sim 10^{12}~{\mathrm{Mpc}}^{-1}$$ k ∼ 10 12 Mpc - 1 , $$10^{8}~{\mathrm{Mpc}}^{-1}$$ 10 8 Mpc - 1 , and $$10^{5}~{\mathrm{Mpc}}^{-1}$$ 10 5 Mpc - 1 , which causes PBHs production in mass scales around $$10^{-13}M_{\odot }$$ 10 - 13 M ⊙ , $$10^{-5}M_{\odot }$$ 10 - 5 M ⊙ , and $$10 M_{\odot }$$ 10 M ⊙ , respectively. Observational constraints confirm that PBHs with a mass scale of $$10^{-13}M_{\odot }$$ 10 - 13 M ⊙ can constitute the total of dark matter in the universe. Furthermore, we estimate the energy density parameter of induced GWs which can be examined by the observation. Also we conclude that it can be parametrized as a power-law function $$\Omega _{\mathrm{GW}}\sim (f/f_c)^n$$ Ω GW ∼ ( f / f c ) n , where the power index equals $$n=3-2/\ln (f_c/f)$$ n = 3 - 2 / ln ( f c / f ) in the infrared limit $$f\ll f_{c}$$ f ≪ f c .

show abstract

Section: Induced Gravitational Wavessupporting

confidence: 55%

Primordial black holes formation in the inflationary model with field-dependent kinetic term for quartic and natural potentials

Solbi

Karami

2021

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

“…For example, the induced GWs from various inflationary models can be found in Refs. [100][101][102][103][104][105][106][107][108][109][110][111][112][113][114][115][116][117][118] and [62,116,119,120] in the context of Higgs inflation. In particular, the large induced GW counterpart to PBH as the totality of dark matter is studied in Refs.…”

Section: Induced Gws Historymentioning

confidence: 99%

“…where we introduced τ from the continuity of the background FLRW metric, i.e., we imposed continuity of a and H at τ = τ rh . Matching (108) and its first derivatives with (106), we find that…”

Section: Matching To Radiation Dominationmentioning

confidence: 99%

Scalar Induced Gravitational Waves Review

2021

View full text Add to dashboard Cite

We provide a review on the state-of-the-art of gravitational waves induced by primordial fluctuations, so-called induced gravitational waves. We present the intuitive physics behind induced gravitational waves and we revisit and unify the general analytical formulation. We then present general formulas in a compact form, ready to be applied. This review places emphasis on the open possibility that the primordial universe experienced a different expansion history than the often assumed radiation dominated cosmology. We hope that anyone interested in the topic will become aware of current advances in the cosmology of induced gravitational waves, as well as becoming familiar with the calculations behind.

show abstract

“…It is understood that, such a rise in scalar power spectrum can be achieved with the aid of a span of USR inflation. Suitable choices of parameters and coupling function between the gravity and derivatives of the scalar field in the NMDC setup can establish such an USR phase due to gravitationally enhanced friction [50][51][52][53][54]. With this regard, in this section we define two-parted form of coupling function θ(φ), to have a correspondence with the available data on large scales (CMB) and a peak in the curvature perturbations on smaller scales, as follows…”

Section: Intensification Of Curvature Perturbations Power Spectrummentioning

confidence: 99%

“…One of the proper ways to achieve a rise in the scalar power spectrum is a brief period of ultra slow-roll (USR) inflation due to declining the speed of inflaton field via gravitationally enhanced friction. The framework of nonminimal derivative coupling to gravity (NMDC) beside the fine-tuning of the parameters of the model can give rise to increase friction gravitationally [50][51][52][53][54][55][56][57][58][59].…”

Section: Introductionmentioning

confidence: 99%

Primordial black holes in nonminimal derivative coupling inflation with quartic potential and reheating consideration

Heydari

Karami

2022

Eur. Phys. J. C

View full text Add to dashboard Cite

We investigate the generation of primordial black holes (PBHs) with the aid of gravitationally increased friction mechanism originated from the nonminimal field derivative coupling (NMDC) to gravity framework, with the quartic potential. Applying the coupling parameter as a two-parted function of inflaton field and fine-tuning of five parameter assortments we can acquire ultra slow-roll phase to slow down the inflaton field due to high friction. This enables us to achieve enough enhancement in the amplitude of curvature perturbations power spectra to generate PBHs with different masses. The reheating stage is considered to obtain criteria for PBHs generation during radiation dominated era. We demonstrate that three cases of asteroid mass PBHs ($$10^{-12}M_{\odot }$$ 10 - 12 M ⊙ , $$10^{-13}M_{\odot }$$ 10 - 13 M ⊙ , and $$10^{-15}M_{\odot })$$ 10 - 15 M ⊙ ) can be very interesting candidates for comprising $$100\%$$ 100 % , $$98.3\%$$ 98.3 % and $$99.1\%$$ 99.1 % of the total dark matter (DM) content of the universe. Moreover, we analyse the production of induced Gravitational Waves (GWs), and illustrate that their spectra of current density parameter $$({\Omega _{{\mathrm{GW}}_\mathrm{0}}})$$ ( Ω GW 0 ) for all parameter Cases foretold by our model have climaxes which cut the sensitivity curves of GWs detectors, ergo the veracity of our outcomes can be tested in light of these detectors. At last, our numerical results exhibit that the spectra of $${\Omega _{{\mathrm{GW}}_\mathrm{0}}}$$ Ω GW 0 behave as a power-law function with respect to frequency, $${\Omega _{{\mathrm{GW}}_\mathrm{0}}} (f) \sim (f/f_c)^{n} $$ Ω GW 0 ( f ) ∼ ( f / f c ) n , in the vicinity of climaxes. Also, in the infrared regime $$f\ll f_{c}$$ f ≪ f c , the power index satisfies the relation $$n=3-2/\ln (f_c/f)$$ n = 3 - 2 / ln ( f c / f ) .

show abstract

Scalar induced gravitational waves in inflation with gravitationally enhanced friction

Cited by 81 publications

References 57 publications

Primordial black holes formation in the inflationary model with field-dependent kinetic term for quartic and natural potentials

Primordial black holes formation in the inflationary model with field-dependent kinetic term for quartic and natural potentials

Scalar Induced Gravitational Waves Review

Primordial black holes in nonminimal derivative coupling inflation with quartic potential and reheating consideration

Contact Info

Product

Resources

About