Searcharxiv⌕ Search
Home/Archive/arXiv

arXiv · 2203.07721

The interaction of neutrinos with Phantom, Quintessence, and Quintum scalar fields and its effect on the formation of structures in the early Universe

Muhammad Yarahmadi·Amin Salehi
View original source ↗Read source document ↗Export metadata ↓

Abstract

Despite the fact that the mass of the neutrinos is so small, they are produced in such vast numbers in the early Universe that their mass induces subtle effects on cosmological observables, primarily the growth of structure and the expansion history in the Universe. We consider the models where neutrino interacts with dark energy scalar field models; phantom, quintessence, and quintom. Also, we obtained the $z_{\rm nr}$ (the redshift at which a mass of neutrino $m_{\nu}$ will become non-relativistic) and surveyed the effect of non-relativistic neutrinos on the structure formation. The data used in this paper are Pantheon + Analysis catalog, CMB, and BAO data. We obtained coupling constant $\beta$ for neutrino and three scalar fields and found that larger $\beta$ values will generally lead to larger neutrino mass in the Universe. For combination data, we found that the total mass of neutrino $\sum m_{\nu}< 0.1197$eV $(95\% $ Confidence Level (C.L.) for quintom model and $\sum m_{\nu}< 0.121 $eV $(95\% $ Confidence Level (C.L.) for phantom model and $\sum m_{\nu}< 0.122$eV $(95\% $ Confidence Level (C.L.) for quintessence model. These results are in broad agreement with the results of Planck 2018 where the total neutrino mass is $\sum m_{\nu}<0.12$eV ($95\%$ C.L., TT, TE, EE+lowE+lensing+BAO). Using the neutrino mass obtained from different models, we calculated $z_{\rm nr}$ and co-moving wave number $k_{\rm nr}$ and showed that neutrinos played a role on the structure formation in the early Universe.

Explore related subjects

gr-qc

Keep this discovery

BibTeXRIS

Muhammad Yarahmadi, Amin Salehi. 2022-03-15. The interaction of neutrinos with Phantom, Quintessence, and Quintum scalar fields and its effect on the formation of structures in the early Universe. https://doi.org/10.1140/epjc%2Fs10052-023-12075-9

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

arXiv2026

Electrovacuum Black Hole Uniqueness

We prove the black hole uniqueness conjecture in the axially symmetric, stationary, electrovacuum setting, subject to the refined asymptotic analysis of the associated singular harmonic maps, which includes an analyticity hypothesis at the axes. More precisely, it is shown that any asymptotically flat solution of the Einstein--Maxwell equations in this class, with more than one black hole horizon component is either: Majumdar--Papapetrou, up to a duality rotation, in which case all logarithmic angle defects vanish, or every finite axis rod logarithmic angle defect is strictly negative and hence every interaction force is strictly attractive. The proof extends the singular harmonic map method used for vacuum Kerr uniqueness in [18].

gr-qc↗
arXiv2026

Constraining Modified Mass-to-Horizon Cosmology Through Primordial Inflationary Observables

We investigate slow-roll inflation in a modified cosmological framework inspired by a generalized mass-to-horizon relation (MHR), $M=\gamma {c^2 L^n}/{G}$, where $n$ is a real parameter and $\gamma$ a dimensional constant. Using Padmanabhan's emergence paradigm, we derive the modified Friedmann equations for a flat FRW universe and analyze the dynamics of a canonical scalar field (inflaton) under the slow-roll approximation. We study the resulting inflationary phenomenology for power-law and Starobinsky potentials. For power-law potentials, the MHR modification fails to reconcile these models with current CMB constraints on $r$ and $n_s$. In contrast, Starobinsky inflation exhibits significant sensitivity to deviations from $n=1$. A perturbative analysis ($n=1+\Delta$) yields corrections to inflationary observables. We observe that the scalar power-spectrum normalization, under a fixed-Starobinsky prescription, imposes the stringent constraint $0.960 \lesssim n \lesssim 1.040$ for $N=60$ efolds. This is considerably tighter than spectral-index bounds. Our results establish inflation, particularly Starobinsky-like models, as a sensitive probe of generalized horizon thermodynamics and departures from standard MHR scaling.

gr-qc↗
arXiv2026

Improving the Sensitivity of Gravitational Wave Detection with Weighted Conformal Prediction

In the last decade, kilometre-scale interferometric gravitational-wave detectors have observed hundreds of compact binary mergers, the majority of which are binary black holes. However, the data are noise-dominated, and multiple independent search algorithms (pipelines) are used to enhance sensitivity and improve robustness. Rather than the standard approach of selecting the most significant pipeline output, we combine the outputs from all pipelines using a conformal prediction-based framework to provide statistically rigorous confidence estimates for candidate events. While combining pipelines improves sensitivity and ranking robustness, it requires a principled statistical framework that remains valid as data properties evolve across observing runs. A key challenge is distribution shifts between simulated datasets used for training and calibration and the real, unlabelled, observations used for testing, which can invalidate coverage guarantees and bias confidence estimates. In this work, we address this challenge by incorporating likelihood-ratio reweighting into our conformal prediction framework to account for covariate shift. Using mock datasets containing simulated signals, we demonstrate that weighted conformal prediction restores well-calibrated coverage under covariate shift and increases the confidence of events near the detection threshold, recovering true signals that would otherwise be missed.

gr-qc↗