Neutrinos as a probe of curvature

Khodagholizadeh, Jafar

doi:10.1016/j.jheap.2021.08.002

Cited by 2 publications

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“…It seems that the presence of curvature will eventually cause a phase difference in the wave number, and this difference should be considered only in low continuous wave numbers. The curvature of the background spacetime in the presence of neutrinos and anti-neutrinos is effective on the amplitude reduction of the primordial gravitational waves [46,58,59]. However, regardless of whether the wave number is discrete or continuous, the time evolution of gravitational waves depends on the value of n, so from now on we can introduce D(t) as D n (t).…”

Section: Linear Field Equation With Dynamic Dark Energymentioning

confidence: 99%

“…However, it is shown that at the temperature of ≈ 10 10 ( 0 K), the tensor modes can be affected by anisotropic inertia, which contains free streaming neutrinos and antineutrinos [3]. This issue has been explored in the spatially curved spacetime and extended to the Λ-dominated era [4][5][6]. Here, we study the effect of dark energy on GWs.…”

Section: Introductionmentioning

confidence: 98%

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Gravitational waves with dark energy

Khodagholizadeh

2022

Journal of High Energy Astrophysics

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Section: Linear Field Equation With Dynamic Dark Energymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Gravitational waves with dark energy

Khodagholizadeh

2022

Journal of High Energy Astrophysics

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Constraints on dark energy from the gravitational wave background

Khodagholizadeh

2023

Eur. Phys. J. C

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Current observational data indicate that dark energy (DE) is a cosmological constant without considering its conclusiveness evidence. Considering the dynamic nature of $$\Lambda $$ Λ individually as a function of time and the scale factor, we review their effects on the gravitational waves. This article is a continuation of the previous work (Khodagholizadeh in JHEAp 36:48–54, 2022), in which DE only was based on Hubble’s parameter and/or its derivatives. For the DE model based on the scale factor ($$a^{-m}$$ a - m ), the results showed that the parameter m is more limited as $$ 2 < m \leqslant 3$$ 2 < m ⩽ 3 compared with the other models and due to the small value of DE density at the early universe. It is only in the mode $$m=3$$ m = 3 that DE affects the low-frequency gravitational waves when its frequency is less than the $$10^{-3}$$ 10 - 3 Hz in a matter-dominated epoch. The broad bound on reducing the amplitude and the B-B polarization multipole coefficients, from maximum to minimum, is for the models developed based on the Hubble parameter function. There are primary sources of low- and very low-frequency GWs, such as the coalescence of massive black hole binaries with $$M_{bh} > 10^{3} M_{sun}$$ M bh > 10 3 M sun , to determine the type of DE by mHz frequency space experiments (e.g., LISA) and by nHz-range NANOGrav 15-year data.

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Neutrinos as a probe of curvature

Cited by 2 publications

References 24 publications

Gravitational waves with dark energy

Gravitational waves with dark energy

Constraints on dark energy from the gravitational wave background

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