Motivated by the first observation of $\rm CP $ violation in baryon decays, we study the topological amplitudes of bottom baryon decays in the $ S U(3)_{\rm F} $ limit. The topological diagrams of the charmless two-body decays of bottom baryons are presented in detail. The linear relations between topologies and $ S U(3) $ irreducible amplitudes are derived through tensor contraction and $ S U(3) $ decomposition. Four amplitudes among the 13 independent amplitudes are critical to the $\rm CP$ asymmetries. The small $ \rm CP $ asymmetries might indicate small relative strong phases between amplitudes $ A_2 $ and $ A_{12,14}^\prime $ . To avoid them, we suggest measuring $\rm CP $ asymmetries in the $ \Xi^0_b\to pK^- $ and $ \Xi^-_b\to \Lambda^0 K^- $ decays. Furthermore, the Körner-Pati-Woo theorem can be tested by measuring the branching fractions of the $ \Lambda_b^0\to\Sigma^0K^0_S $ and $ \Lambda_b^0\to\Sigma^-K^+ $ modes.

China

Di Wang

Wei-Chen Fu

Topological amplitudes of bottom baryon decays in the $\textit{SU}$(3)$_{F}$ limit * Supported in part by the National Natural Science Foundation of China (12105099)

We use a modified relativistic quark model to study the properties of excited charmed and charmed strange mesons. We calculate the masses and wave functions of conventional charmed and charmed strange mesons incorporating both spin and $\textit{S}$-$\textit{D}$ mixing effects and fit parameters of the potential model with known experimental states using differential evolution techniques. Using leading Born-Oppenheimer expansion, we compute the spectrum and wave functions of the first gluonic excited state of charmed and charmed strange mesons. We examine the effects of gluonic excitation on the spectrum of the resulting hybrid mesons. Using our calculated spectrum and wave functions, we determine the radiative transitions of the conventional and hybrid open charm mesons. We compare our calculations with experimental data and other works. We expect our results will be beneficial in the detection of charmed and charmed strange conventional and hybrid mesons.

Pakistan

Saba Noor

Faisal Akram

Bilal Masud

Study of excited $\textit{D}$ and D$_{s}$ mesons in a relativized quark model * F. A. acknowledges HEC grant 20-15728/NRPU/R&D/HEC/2021, Pakistan

Nucleon structure functions, as measured in lepton-nucleon scattering, have historically provided a critical observable in the study of partonic dynamics within the nucleon. However, at very large parton momenta, it is both experimentally and theoretically challenging to extract parton distributions due to the probable onset of nonperturbative contributions and the unavailability of high-precision data at critical kinematics. Extraction of the neutron structure and the d quark distribution have been further challenging because of the necessity of applying nuclear corrections when utilizing scattering data from a deuteron target to extract the free neutron structure. However, a program of experiments has been carried out recently at the energy-upgraded Jefferson Lab electron accelerator aimed at significantly reducing the nuclear correction uncertainties on the d quark distribution function at large partonic momentum. This allows leveraging the vast body of deuterium data covering a large kinematic range to be utilized for d quark parton distribution function extraction. In this Letter, we present new data from experiment E12-10-002, carried out in Jefferson Lab Experimental Hall C, on the deuteron to proton cross section ratio at large Bjorken <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi>x</mi></mrow></math>. These results significantly improve the precision of existing data and provide a first look at the expected impact on quark distributions extracted from parton distribution function fits.

United States

D. Biswas

F.A. Gonzalez

W. Henry

A. Karki

C. Morean

A. Nadeeshani

A. Sun

Canada

Z. Ahmed

Saudi Arabia

S. Alsalmi

W. Armstrong

A. Asaturyan

C. Ayerbe Gayoso

V. Berdnikov

H. Bhatt

D. Bhetuwal

P. Bosted

E. Brash

M.H.S. Bukhari

J.P. Chen

M. Chen

M.E. Christy

S. Covrig Dusa

K. Craycraft

S. Danagoulian

D. Day

M. Diefenthaler

M. Dlamini

J. Dunne

B. Duran

D. Dutta

R. Ent

H. Fenker

N. Fomin

E. Fuchey

D. Gaskell

T.N. Gautam

J.O. Hansen

F. Hauenstein

A.V. Hernandez

T. Horn

G.M. Huber

M.K. Jones

S. Joosten

M.L. Kabir

C. Keppel

A. Khanal

P.M. King

E. Kinney

M. Kohl

N. Lashley-Colthirst

S. Li

W.B. Li

A.H. Liyanage

D. Mack

S. Malace

P. Markowitz

J. Matter

D. Meekins

R. Michaels

Armenia

A. Mkrtchyan

H. Mkrtchyan

Z. Moore

S.J. Nazeer

S. Nanda

G. Niculescu

I. Niculescu

D. Nguyen

 Nuruzzaman

B. Pandey

S. Park

E. Pooser

A.J.R. Puckett

M. Rehfuss

J. Reinhold

B. Sawatzky

G.R. Smith

H. Szumila-Vance

A.S. Tadepalli

V. Tadevosyan

R. Trotta

S.A. Wood

C. Yero

J. Zhang

New Measurements of the Deuteron-to-Proton <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>F</mi></mrow><mrow><mn>2</mn></mrow></msub></mrow></math> Structure-Function Ratio

Axionlike particles (ALPs), hypothetical particles beyond the Standard Model (SM), are considered as promising dark matter candidates. ALPs can convert into photons and vice versa in a magnetic field via the Primakoff effect, potentially generating detectable oscillation in <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>γ</mi></math>-ray spectra. This study analyzes 16.5 years of data from the Fermi Large Area Telescope (Fermi-LAT) on NGC 1275, the brightest galaxy in the Perseus cluster, to constrain the ALP parameter space. Our results improve the previous 95% exclusion limits of the photon-ALP coupling <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub></math> by a factor of 2 in the ALP mass range of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>4</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>10</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi><mo>≲</mo><msub><mi>m</mi><mi>a</mi></msub><mo>≲</mo><mn>5</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>9</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>. Moreover, we investigate the projected sensitivity of the future Very Large Area <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>γ</mi></math>-ray Space Telescope (VLAST) on searching for ALPs. We find that (i) the expected sensitivity on the photon-ALP coupling <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub></math> can be stronger than that from the upcoming International Axion Observatory in the ALP mass range of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>2</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>11</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi><mo>≲</mo><msub><mi>m</mi><mi>a</mi></msub><mo>≲</mo><mn>1</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>7</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>, with the best sensitivity of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub><mo>∼</mo><mn>7</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>13</mn></mrow></msup><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> at <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>m</mi><mi>a</mi></msub><mo>∼</mo><mn>2</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>10</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>; (ii) VLAST can extend the sensitivity of the ALP masses below <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>5</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>12</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>, where the photon-ALP coupling <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub><mo>≳</mo><mn>1.5</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>11</mn></mrow></msup><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> will be excluded; (iii) the entire parameter space of ALP accounting for TeV transparency can be fully tested. These results demonstrate that VLAST will offer an excellent opportunity for ALPs searches.

Zhi-Qi Guo

Yue-Lin Sming Tsai

Lei Wu

Zi-Qing Xia

Constraints on axionlike particles from 16.5 years of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>F</mi><mi>e</mi><mi>r</mi><mi>m</mi><mi>i</mi></math>-LAT data and prospects for VLAST

$\textit{f}$($\textit{Q}$) and $\textit{f}$($\textit{T}$) gravity are based on fundamentally different geometric frameworks, yet they exhibit many similar properties. This article provides a comprehensive summary and comparative analysis of the various theoretical branches of torsional gravity and non-metric gravity, which arise from different choices of affine connection. We identify two types of background-dependent and classical correspondences between these two theories of gravity. The first correspondence is established through their equivalence within the Minkowski spacetime background. To achieve this, we develop the tetrad-spin formulation of $\textit{f}$($\textit{Q}$) gravity and derive the corresponding expression for the spin connection. The second correspondence is based on the equivalence of their equations of motion. Utilizing a metric-affine approach, we derive the general affine connection for static and spherically symmetric spacetime in $\textit{f}$($\textit{Q}$) gravity and compare its equations of motion with those of $\textit{f}$($\textit{T}$) gravity. Among others, our results reveal that, $\textit{f}$($\textit{T}$) solutions are not simply a subset of $\textit{f}$($\textit{Q}$) solutions; rather, they encompass a complex solution beyond $\textit{f}$($\textit{Q}$) gravity in black hole background.

Cheng Wu

Japan

Xin Ren

Yuhang Yang

Yu-Min Hu

Chile

Greece

Emmanuel Saridakis

Background-dependent and classical correspondences between $\textit{f}$($\textit{Q}$) and $\textit{f}$($\textit{T}$) gravity

In this article, we develop two unique singularity-free solutions that describe anisotropic interior fluid configurations in <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity. In this regard, the extended field equations are developed corresponding to a static interior spacetime. This system of equations is facilitated by imposing two novel constraints in order to get a unique solution. We derive two different solutions by choosing specific types of anisotropic pressure. While solving these equations, several constants are involved as a result of performing exact integration. Matching the interior metric to the Schwarzschild exterior metric at the sphere&#8217;s boundary in both scenarios yields these integration constants. Another factor that plays an important role in finding the constants is the zero radial pressure. Afterwards, physical feasibility of both compact models is explored under specific conditions. To do so, the predicted data of two stars, named 4U 1820-30 and Cen X-3 is used along with different values of the model parameter. It is reported that both our astrophysical solutions are aligned with the criteria of physical existence of such models under certain parametric values.

Azerbaijan

Tayyab Naseer

M. Sharif

M. Waqas

Mohamed R. Eid

Abdel-Haleem Abdel-Aty

Astrophysical stellar models in <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity under Tolman IV and Kohler-Chao-Tikekar spacetimes

In this paper, we investigate the helicity form factors (HFFs) of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mrow><mo stretchy="false">(</mo><mi>s</mi><mo stretchy="false">)</mo></mrow></msub></math>-meson decay into a scalar meson with a mass larger than 1 GeV, i.e., <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>B</mi><mo stretchy="false">→</mo><msub><mi>a</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1450</mn><mo stretchy="false">)</mo></math>, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mrow><mo stretchy="false">(</mo><mi>s</mi><mo stretchy="false">)</mo></mrow></msub><mo stretchy="false">→</mo><msubsup><mi>K</mi><mn>0</mn><mo>*</mo></msubsup><mo stretchy="false">(</mo><mn>1430</mn><mo stretchy="false">)</mo></math>, and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mi>s</mi></msub><mo stretchy="false">→</mo><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1500</mn><mo stretchy="false">)</mo></math> by using the light-cone sum rules approach. We take the standard currents for correlation functions. To enhance the precision of our calculations, we incorporate the next-to-leading order (NLO) corrections and retain the scalar meson twist-3 light-cone distribution amplitudes. Furthermore, we extend the HFFs to the entire physical <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>q</mi><mn>2</mn></msup></math> region employing a simplified <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>z</mi></math>-series expansion. At the point of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mi>q</mi></mrow><mn>2</mn></msup><mo>=</mo><mn>1</mn><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mn>2</mn></msup></mrow></math>, all NLO contributions to the HFFs are negative, with the maximum contribution around 25%. Then, as applications of these HFFs, we analyze the differential decay widths, branching ratios, and lepton polarization asymmetries for the semileptonic <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mrow><mo stretchy="false">(</mo><mi>s</mi><mo stretchy="false">)</mo></mrow></msub><mo stretchy="false">→</mo><mi>S</mi><mo>ℓ</mo><msub><mover accent="true"><mi>ν</mi><mo stretchy="false">¯</mo></mover><mo>ℓ</mo></msub></math>, FCNC <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mrow><mo stretchy="false">(</mo><mi>s</mi><mo stretchy="false">)</mo></mrow></msub><mo stretchy="false">→</mo><mi>S</mi><mo>ℓ</mo><mover accent="true"><mo>ℓ</mo><mo stretchy="false">¯</mo></mover></math> and rare <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mrow><mo stretchy="false">(</mo><mi>s</mi><mo stretchy="false">)</mo></mrow></msub><mo stretchy="false">→</mo><mi>S</mi><mi>ν</mi><mover accent="true"><mi>ν</mi><mo stretchy="false">¯</mo></mover></math> decays. Our results are consistent with existing studies within uncertainties. The current data still suffer from large uncertainties and need to be measured more precisely, which can lead to a better understanding of the fundamental properties of light scalar mesons.

Yi Zhang

Wei Cheng

Jia-Wei Zhang

Tao Zhong

Hai-Bing Fu

Li-Sheng Geng

<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>B</mi><mrow><mo stretchy="false">(</mo><mi>s</mi><mo stretchy="false">)</mo></mrow></msub><mo stretchy="false">→</mo><mi>S</mi><mo stretchy="false">(</mo><msub><mi>a</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1450</mn><mo stretchy="false">)</mo><mo>,</mo><mtext> </mtext><msubsup><mi>K</mi><mn>0</mn><mo>*</mo></msubsup><mo stretchy="false">(</mo><mn>1430</mn><mo stretchy="false">)</mo><mo>,</mo><mtext> </mtext><mtext> </mtext><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1500</mn><mo stretchy="false">)</mo><mo stretchy="false">)</mo></math> helicity form factors within QCD light-cone sum rules

This paper investigates the late-time cosmic dynamics using the matter-geometry coupled <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity model, where <math altimg='si82.svg'><mi>Q</mi></math> is the non-metricity scalar and <math altimg='si83.svg'><mi>T</mi></math> represents the trace of the energy-momentum tensor. We consider the paradigm power law <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math>-gravity model, <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> = - <math altimg='si84.svg'><mrow><mi>&#945;</mi><mi>Q</mi><mo linebreak='goodbreak'>&#8722;</mo><mi>&#946;</mi><msup><mi>T</mi><mn>2</mn></msup><mo linebreak='goodbreak'>/</mo><msubsup><mi>H</mi><mn>0</mn><mn>2</mn></msubsup><mo linebreak='goodbreak'>+</mo><msub><mi>&#951;</mi><mn>0</mn></msub></mrow></math> (where <math altimg='si8.svg'><mi>&#945;</mi></math>, <math altimg='si9.svg'><mi>&#946;</mi></math> and <math altimg='si85.svg'><msub><mi>&#951;</mi><mn>0</mn></msub></math> are constants) to calculate the best-fit values of cosmological parameters <math altimg='si7.svg'><msub><mstyle mathvariant='normal'><mi>&#937;</mi></mstyle><mi>m</mi></msub></math>, <math altimg='si3.svg'><msub><mi>H</mi><mn>0</mn></msub></math>, <math altimg='si8.svg'><mi>&#945;</mi></math>, <math altimg='si9.svg'><mi>&#946;</mi></math>, <math altimg='si15.svg'><msub><mi>r</mi><mi>d</mi></msub></math> and <math altimg='si16.svg'><mi>M</mi></math> through the Monte Carlo Markov Chain (MCMC) simulations using cosmic chronometers (CC) baryon acoustic oscillation (BAO) taken from Dark Energy Spectroscopy Instrument (DESI) and the SNIa distance moduli measurements from the Pantheon + SH0ES, which consists of 1701 light curves of 1550 distinct supernovae. Some key cosmological parameters: the deceleration parameter <math altimg='si4.svg'><mrow><mi>q</mi><mo>(</mo><mi>z</mi><mo>)</mo></mrow></math>, effective equation of state parameters <math altimg='si86.svg'><mrow><msub><mi>w</mi><mrow><mi>e</mi><mi>f</mi><mi>f</mi></mrow></msub><mrow><mo>(</mo><mi>z</mi><mo>)</mo></mrow></mrow></math>, Hubble parameter <math altimg='si10.svg'><mrow><mi>H</mi><mo>(</mo><mi>z</mi><mo>)</mo></mrow></math>, and distance modulus <math altimg='si87.svg'><mrow><mi>&#956;</mi><mo>(</mo><mi>z</mi><mo>)</mo></mrow></math> are presented. These dynamical quantities show that the <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math>-gravity model is compatible with transitioning towards a quintessence-like phase in the late-time. In conformity with <math altimg='si5.svg'><mstyle mathvariant='normal'><mi>&#923;</mi></mstyle></math>CDM, we moreover take into account the geometrical interpretations by considering the state-finder parameters <math altimg='si11.svg'><mrow><mi>r</mi><mo linebreak='goodbreak'>&#8722;</mo><mi>s</mi></mrow></math> and <math altimg='si12.svg'><mrow><mi>r</mi><mo linebreak='goodbreak'>&#8722;</mo><mi>q</mi></mrow></math>, which are crucial parameters for additional analysis. Additionally, the statistical analysis has been carried out for further investigation of the viability <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math>-gravity model.

South Africa

Shambel Sahlu

India

B.K. Shukla

R.K. Tiwari

Türkiye

Değer Sofuoğlu

Alnadhief H A Alfedeel

Quintessence phase of the universe in <math altimg='si6.svg'><mrow><mi>f</mi><mo>(</mo><mi>Q</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math>-gravity with <italic>DESI DR2 BAO</italic> and <italic>Pantheon + SH0ES</italic> samples

In this study, we construct a traversable wormhole solution within the framework of <math altimg='si16.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity by assuming conformal symmetry. The matter content is modeled using phantom energy, characterized by an equation of state parameter <math altimg='si17.svg'><mrow><mi>&#969;</mi><mo linebreak='goodbreak'>&lt;</mo><mo>&#8722;</mo><mn>1</mn></mrow></math>, which inherently violates the null energy condition. By employing conformal Killing vector symmetry, we derive exact analytical expressions for the shape function, energy density, and pressure components of the anisotropic fluid. Our analysis includes a detailed examination of the flare-out condition, proper radial distance, embedding diagrams, and the generalized Tolman-Oppenheimer-Volkoff equation. Notably, the model yields a positive active gravitational mass and positive total gravitational energy, despite the presence of exotic matter.

Doğukan Taşer

Existence of conformal symmetric wormhole with phantom energy in <math altimg='si16.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> theory

In this study, we investigate the viability of the <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity framework in explaining the accelerated expansion of the universe within the context of the locally rotationally symmetric (LRS) Bianchi-I space-time. Modified gravity theories have emerged as promising alternatives to General Relativity (GR) to account for cosmic acceleration and dark energy phenomena. We employ observational constraints from Type Ia Supernovae (SN Ia), Baryon Acoustic Oscillations (BAO), and Cosmic Chronometers (CC) to calibrate the free parameters of our model. The field equations are formulated based on a specific functional form of <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math>, and analytical solutions are obtained. The Hubble parameter, deceleration parameter ( <math altimg='si10.svg'><mi>q</mi></math>), statefinder diagnostics <math altimg='si74.svg'><mrow><mo>(</mo><mi>r</mi><mo>,</mo><mi>s</mi><mo>)</mo></mrow></math>, and the jerk parameter ( <math altimg='si12.svg'><mi>j</mi></math>) are utilized to analyze the evolutionary dynamics of the universe. Our results indicate a transition from a decelerating to an accelerating phase, with the transition redshift <math altimg='si75.svg'><mrow><msub><mi>z</mi><mi>t</mi></msub><mo linebreak='goodbreak'>=</mo><mn>0</mn><mo>.</mo><msubsup><mn>7293</mn><mrow><mo>&#8722;</mo><mn>0.06</mn></mrow><mrow><mo>+</mo><mn>0.07</mn></mrow></msubsup></mrow></math> and present deceleration parameter <math altimg='si76.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo linebreak='goodbreak'>=</mo><mo>&#8722;</mo><mn>0.56</mn></mrow></math>, consistent with observational data. The estimated age of the universe in this framework is <math altimg='si77.svg'><mrow><mn>13.27</mn><mo>&#177;</mo><mn>0.26</mn></mrow></math> Gyrs. The statefinder parameters suggest that the model closely mimics the standard <math altimg='si5.svg'><mstyle mathvariant='normal'><mi>&#923;</mi></mstyle></math>CDM scenario at present but exhibits deviations at earlier epochs, potentially indicating a dynamic nature of dark energy. The <math altimg='si78.svg'><msub><mi>O</mi><mi>m</mi></msub></math> diagnostic further confirms the compatibility of our model with a phantom-like behavior of dark energy. These findings support the viability of <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity as an alternative framework for explaining cosmic acceleration, providing new interplay between matter and curvature in gravitational dynamics.

Vinod Kumar Bhardwaj

Anil Kumar Yadav

S.H. Shekh

Constraining <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity with SN Ia and BAO observational data in Bianchi I space time