arXiv subjects

Yash B. Ingole

Publications and source records attributed to Yash B. Ingole.

5 recordsLinked to original sources

arXiv2025

Exploring Dark Energy via Non-Minimal Coupling in $f(Q,L_m)$ Gravity with Gong-Zhang Parameterization

In this study, we investigate the late-time accelerated expansion of the universe within the framework of non-minimally coupled $f(Q,L_m)$ gravity, where $Q$ is the non-metricity scalar and $L_m$ is the matter Lagrangian. We derive modified Friedmann equations in a flat FLRW background and employ the \textit{Gong-Zhang} parameterization for the DE equation of state (EoS), allowing an analytical form of the Hubble parameter $H(z)$. The model parameters are constrained using recent Cosmic Chronometers (CC) and Pantheon+SH0ES Type Ia supernova datasets through MCMC-based chi-squared minimization. We analyze various cosmological quantities including the deceleration parameter, EoS, jerk, snap, lerk, and diagnostic tools such as $Om(z)$ and the statefinder pair $(r,s)$. Our findings indicate a viable transition from deceleration to acceleration and reveal a quintessence-to-phantom-like evolution of dark energy. Furthermore, energy conditions are examined, showing a violation of the strong energy condition, consistent with current cosmic acceleration. The results establish that the $f(Q,L_m) $ framework with non-minimal coupling and parameterized EoS provides a compelling alternative to $Λ$CDM in describing cosmic acceleration.

gr-qc↗

arXiv2025

Parameterized Deceleration in $f(Q,C)$ Gravity: A Logarithmic Approach

This study explores a distinctive logarithmic parameterization of the deceleration parameter within the $f(Q, C)$ gravity framework, incorporating a nonlinear functional form $f(Q, C) = γ_1 Q^n + γ_2 C$, where $Q$ and $C$ denote the nonmetricity scalar and boundary term, respectively, and $n \geq 1$. This approach provides a unique perspective on the universe's accelerated expansion without resorting to exotic fields. Using observational data from Hubble measurements (OHD) and the Pantheon+SH0ES Type Ia supernovae dataset, the model parameters were constrained through a $χ^2$ minimization technique. The analysis reveals a transition from deceleration to acceleration in the expansion history of the universe, with the transition redshifts $z_t \approx 0.98$ (OHD) and $z_t \approx 0.76$ (Pantheon+SH0ES). The model demonstrates consistency with observations, offering insights into the dynamics of dark energy and alternative gravity theories, while effectively modeling cosmic evolution across epochs.

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arXiv2024

Generalized Ghost Pilgrim Dark Energy Fractal Cosmology with Observational Constraint

In this work, we explore dark energy models, mainly ghost, generalized ghost, and generalized ghost pilgrim dark energy models within the framework of fractal cosmology. To obtain solutions for the field equations, we employ a parameterization of the deceleration parameter as proposed by \textit{R.K. Tiwari}. By utilizing Markov Chain Monte Carlo (MCMC) analysis, we impose constraints on the free parameters of the derived solutions. The analysis is based on observational datasets, including 57 data points from the Observational Hubble Data ($OHD$) and, 1048 points from the $Pantheon$ Supernovae sample. This approach allows us to assess the viability of the dark energy models in describing the current cosmic expansion. According to the effective equation-of-state parameter, the model maintains itself in the quintessence era and ultimately switches into the Einstein-de Sitter model. Furthermore, we investigate the statefinder, jerk, snap, and lerk parameters. The energy conditions of each model satisfy the weak and null energy conditions but violate the strong energy condition. We find that the $Om(z)$ curves for the data samples exhibit a consistently negative slope throughout the entire range.

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arXiv2024

Resolving FLRW cosmology through effective equations of state in $f(T)$ gravity

This article explores the cosmological scenario of the universe in the context of the $f(T)$ power law model, where $T$ represent the torsion scalar. To obtain the deterministic solution of the field equations we parametrized the effective Equation-of-State with two parameters $m$ and $k$ as suggested by A. Mukherjee in a flat FLRW environment. We impose constraints on the free parameters of the derived solution by utilizing MCMC analysis assuming the $CC, Pantheon+SH0ES$, and $CC+Pantheon+SH0ES$ as data samples. We explore the dynamics of cosmological parameters. The evolutionary profile of the deceleration parameter exhibits the transition %from the decelerated to the accelerated phase. The effective Equation-of-State parameter indicates the model remains in the quintessence era and gradually becomes the Einsteins-de-Sitter model. In addition to this, we also explore the jerk, snap, and lerk parameters. Furthermore, the $Om(z)$ diagnostic shows that the model has a consistent positive slope across the entire evolution, but resembles the standard $Λ$CDM model in the near future. At last, we conclude that the power law function of the modified $f(T)$ gravity model in the framework of the FLRW universe aligns more closely with the $Λ$CDM model for given observational data.

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arXiv2024

Cosmic Evolution of the Kantowski-Sachs Universe in the Context of a Bulk Viscous String in Teleparallel Gravity

In the present work, we analyzed the Kantowski-Sachs cosmological model along with teleparallel gravity, where a bulk viscous fluid containing one-dimensional cosmic strings serves as the source for the energy$-$momentum tensor. To obtain the deterministic solution of the field equations, we employed the proportionality condition linking the shear scalar $(σ)$ and the expansion scalar $(θ)$, establishing a relationship between metric potentials. Another approach employed is the utilization of the hybrid expansion law (HEL). The discussion focuses on the behavior of the accelerating universe concerning the specific choice of a nonlinear (or power law model) of teleparallel gravity $f(T)=αT + βT^m$, where $T$ is the torsion scalar, $α$ , and $β$ are model parameters and $m$ is restricted to greater than or equal to 2. The effective equation of the state parameter $(ω_{eff})$ of models support the acceleration of the universe. We observed that the null energy condition and weak energy condition are obeyed but violate the strong energy condition as per the present accelerating expansion. Under specific model parameter constraints, the universe shows a transition from a decelerating to an accelerating phase.

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