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

In this article we propose the scheme of integration of two-dimensional $\textit{F}$($\textit{R}$) gravity vacuum equations in a travelling wave variable. The main emphasis is placed on the fundamental possibility of obtaining different forms of the function $\textit{F}$($\textit{R}$) by arbitrarily choosing a certain function through which all components of the metric tensor of the theory can be expressed.

Russia

Maria Shubina

Scheme of integration of vacuum $\textit{F}$($\textit{R}$) gravity in a travelling wave variable

The isospin-singlet scalar meson <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math> is hypothesized to consist of two energy eigenstates, forming a mixture of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mfrac><mn>1</mn><msqrt><mn>2</mn></msqrt></mfrac><mo stretchy="false">(</mo><mover accent="true"><mi>u</mi><mo stretchy="false">¯</mo></mover><mi>u</mi><mo>+</mo><mover accent="true"><mi>d</mi><mo stretchy="false">¯</mo></mover><mi>d</mi><mo stretchy="false">)</mo></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mover accent="true"><mi>s</mi><mo stretchy="false">¯</mo></mover><mi>s</mi></math>. Building on this framework, we apply the quantum chromodynamics (QCD) sum rules approach in the background field theory to compute the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math> decay constant, yielding <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><msub><mi>f</mi><mn>0</mn></msub></msub><mo stretchy="false">(</mo><msub><mi>μ</mi><mn>0</mn></msub><mo>=</mo><mn>1</mn><mtext> </mtext><mtext> </mtext><mi>GeV</mi><mo stretchy="false">)</mo><mo>=</mo><mn>0.386</mn><mo>±</mo><mn>0.009</mn><mtext> </mtext><mtext> </mtext><mi>GeV</mi></math>. Subsequently, we derive the first two <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>ξ</mi></math>-moments of the leading-twist light-cone distribution amplitude <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>ϕ</mi><mrow><mn>2</mn><mo>;</mo><msub><mi>f</mi><mn>0</mn></msub></mrow></msub></math>. Using QCD light-cone sum rules, we then calculate the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>D</mi><mi>s</mi><mo>+</mo></msubsup><mo stretchy="false">→</mo><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math> transition form factor (TFF) <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mo>+</mo></msub><mo stretchy="false">(</mo><msup><mi>q</mi><mn>2</mn></msup><mo stretchy="false">)</mo></math>, obtaining <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mo>+</mo></msub><mo stretchy="false">(</mo><mn>0</mn><mo stretchy="false">)</mo><mo>=</mo><mn>0.51</mn><msubsup><mn>6</mn><mrow><mo>−</mo><mn>0.024</mn></mrow><mrow><mo>+</mo><mn>0.027</mn></mrow></msubsup></math> at the large-recoil region. We extend <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mo>+</mo></msub><mo stretchy="false">(</mo><msup><mi>q</mi><mn>2</mn></msup><mo stretchy="false">)</mo></math> to the full physical region via a simplified series expansion parametrization, enabling calculations of the differential decay widths and the branching fraction <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi mathvariant="script">B</mi><mo stretchy="false">(</mo><msubsup><mi>D</mi><mi>s</mi><mo>+</mo></msubsup><mo stretchy="false">→</mo><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo><mo stretchy="false">(</mo><mo stretchy="false">→</mo><msup><mi>π</mi><mo>+</mo></msup><msup><mi>π</mi><mo>−</mo></msup><mo stretchy="false">)</mo><msup><mi>e</mi><mo>+</mo></msup><msub><mi>ν</mi><mi>e</mi></msub><mo stretchy="false">)</mo><mo>=</mo><mspace linebreak="goodbreak"></mspace><mo stretchy="false">(</mo><mn>1.78</mn><msubsup><mn>3</mn><mrow><mo>−</mo><mn>0.189</mn></mrow><mrow><mo>+</mo><mn>0.227</mn></mrow></msubsup><mo stretchy="false">)</mo><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>3</mn></mrow></msup></math>. Our theoretical predictions align well with the latest BESIII Collaboration measurements within reasonable errors.

Dan-Dan Hu

Xing-Gang Wu

Hai-Jiang Tian

Tao Zhong

Hai-Bing Fu

Light-cone sum rules analysis of the semileptonic <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>D</mi><mi>s</mi><mo>+</mo></msubsup><mo stretchy="false">→</mo><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo><mspace linebreak="goodbreak"></mspace><mo stretchy="false">(</mo><mo stretchy="false">→</mo><msup><mi>π</mi><mo>+</mo></msup><msup><mi>π</mi><mo>−</mo></msup><mo stretchy="false">)</mo><msup><mi>e</mi><mo>+</mo></msup><msub><mi>ν</mi><mi>e</mi></msub></math> decay incorporating the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math> mixing state twist-2 distribution amplitudes

We introduce <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>w</mi><mi>i</mi></msub><msub><mi>f</mi><mi>i</mi></msub></math> ensembles as a novel framework to obtain asymptotic frequentist uncertainties on density ratios, with a particular focus on neural ratio estimation in the context of high-energy physics. When the density ratio of interest is a likelihood ratio conditioned on parameters, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>w</mi><mi>i</mi></msub><msub><mi>f</mi><mi>i</mi></msub></math> ensembles can be used to perform simulation-based inference on those parameters. After training the basis functions <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mi>i</mi></msub><mo stretchy="false">(</mo><mi>x</mi><mo stretchy="false">)</mo></math>, uncertainties on the weights <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>w</mi><mi>i</mi></msub></math> can be straightforwardly propagated to the estimated parameters without requiring extraneous bootstraps. To demonstrate this approach, we present an application in quantum chromodynamics at the Large Hadron Collider, using <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>w</mi><mi>i</mi></msub><msub><mi>f</mi><mi>i</mi></msub></math> ensembles to estimate the likelihood ratio between generated quark and gluon jets. We use this learned likelihood ratio to estimate the quark fraction in a synthetic mixed quark/gluon sample, showing that the resultant uncertainties empirically satisfy the desired coverage properties.

United States

Sean Benevedes

Jesse Thaler

Frequentist uncertainties on neural density ratios with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>w</mi><mi>i</mi></msub><mtext> </mtext><msub><mi>f</mi><mi>i</mi></msub></math> ensembles

In this work, we explore a cosmological model within the framework of modified gravity, specifically a logarithmic form of $\textit{f}$($\textit{Q}$) gravity. Using recent observational datasets including RSD and DESI, we constrain the model parameters via Markov Chain Monte Carlo (MCMC) techniques. Our analysis focuses on both background and perturbation-level cosmological diagnostics, evaluating the evolution of cosmographic parameters and the growth rate of structure through $$f\sigma _8$$ . The results demonstrate consistency with observational data, particularly supporting a quintessence-like accelerated expansion. Additionally, the model addresses the $$S_8$$ tension and provides insights into the late-time behavior of dark energy.

India

L. Sudharani

N. Kavya

V. Venkatesha

Cosmic structure growth and perturbation analysis in logarithmic $\textit{f}$($\textit{Q}$) gravity

We construct an analytic $\textit{f}$($\textit{R}$) gravity model that unifies early-time inflation with late-time cosmic acceleration within a single covariant framework. At high curvature, the model reproduces a Starobinsky-like inflationary plateau, while at low curvature it asymptotes to a stable dark energy-dominated phase. In the scalar-tensor representation, this construction yields a hilltop-type potential in the Jordan frame, which maps to an exponential potential in the Einstein frame. To account for radiative effects, we introduce a logarithmic correction to the Einstein-frame potential inspired by one-loop effective field theory, producing a late-time flattening without requiring fine-tuning. The resulting scalaron dynamics reduce the effective mass to $$\mathcal {O}(H_0)$$ , inducing a thawing regime that deviates from a cosmological constant at the sub-percent levels. A joint background likelihood analysis using Pantheon+SH0ES and BAO+CC datasets (within the CPL parametrization) yields $$H_0 = 73.4 \pm 0.6$$ km/s/Mpc and $$\Omega _m = 0.253 \pm 0.007$$ , consistent with local expansion rate measurements. The best-fit scalar field parameters are $$\varphi _0 \approx 0.027\,M_\textrm{Pl}$$ and $$\lambda \approx 0.010\,M_\textrm{Pl}$$ , corresponding to a present-day dark energy equation of state $$w_0 \approx -0.985$$ . While compatible with $$\Lambda $$ CDM within current observational bounds, the model satisfies GR recovery at low curvature and exhibits attractor-like behavior, thereby minimizing sensitivity to initial conditions.

M. Pradosh Keshav

Arun Kenath

Loop-corrected scalar potentials and late-time acceleration in $$f(R)$$ gravity

In this paper, we present intriguing traversable and asymptotically flat wormhole solutions within <math altimg='si18.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. We integrate our model with the gravitational analog of the Schwinger effect, describing the emergence of particle-antiparticle pairs from the vacuum. By introducing a fundamental minimal length via the generalized uncertainty principle, we establish critical constraints on matter distribution and spacetime structure. Our findings reveal how this fundamental length shapes the wormhole geometry, steepening the slope toward the throat and mitigating violations of the weak and null energy conditions. This adjustment allows the supporting matter to avoid phantom behavior at the Planck scale, suggesting a more stable configuration. We also explore the intriguing effects of gravitational lensing, showing that these exotic wormholes repel light rather than capture it. For <math altimg='si9.svg'><mi>&#946;</mi></math> values ranging from 0 to 45, the deflection angle remains negative for all corresponding <math altimg='si14.svg'><mrow><mi>&#945;</mi><mo>(</mo><msub><mi>r</mi><mrow><mi>t</mi><mi>p</mi></mrow></msub><mo>)</mo></mrow></math> values, indicating a repulsive gravitational force that pushes photons away from the throat. Moreover, the forces acting on the wormhole exhibit a delicate balance, demonstrating equal strength in opposing directions&#8211;an essential feature of stability. The complexity factor <math altimg='si17.svg'><msub><mi>Y</mi><mrow><mi>T</mi><mi>F</mi></mrow></msub></math> decreases with distance from the throat, indicating that corrections from the generalized uncertainty principle are most significant near the throat and diminish outward. Overall, our work highlights the allure of these wormhole geometries and the pivotal role of quantum effects in their formation, paving new avenues for understanding gravity and spacetime.

South Africa

Azerbaijan

A. Errehymy

Uzbekistan

B. Turimov

Kazakhstan

A. Syzdykova

K. Myrzakulov

Saudi Arabia

N. Alessa

A.H. Abdel-Aty

Dymnikova-Schwinger GUP-corrected wormholes in <math altimg='si18.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

Motivated by the recent BESIII Collaboration measurements of the decay <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>D</mi><mo>+</mo></msup><mo stretchy="false">→</mo><msup><mi>π</mi><mo>+</mo></msup><mi>η</mi><mi>η</mi></math>, we investigate this process by considering the contribution from the resonance <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>a</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math>, which is generated by <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>S</mi></math>-wave pseudoscalar meson-pseudoscalar meson interaction, and the contribution from the intermediate scalar meson <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1370</mn><mo stretchy="false">)</mo></math>. Our results could give a good description of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>π</mi><mo>+</mo></msup><mi>η</mi></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>η</mi><mi>η</mi></math> invariant mass distributions, which implies that the contribution from the intermediate <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1370</mn><mo stretchy="false">)</mo></math>, neglected in BESIII analysis, could play a role in this process. Furthermore, the predicted Dalitz plots are also consistent with the BESIII measurements. The more precise measurements about this process in the future could shed light on the mechanism of this process and the properties of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1370</mn><mo stretchy="false">)</mo></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>a</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math>.

Wen-Tao Lyu

Le-Le Wei

De-Min Li

En Wang

Hadronic decay <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>D</mi><mo>+</mo></msup><mo stretchy="false">→</mo><msup><mi>π</mi><mo>+</mo></msup><mi>η</mi><mi>η</mi></math> and the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>a</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>980</mn><mo stretchy="false">)</mo></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mn>0</mn></msub><mo stretchy="false">(</mo><mn>1370</mn><mo stretchy="false">)</mo></math> contributions

We examine inflationary models in the <math altimg='si1.svg'><mi>f</mi><mo stretchy='false'>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo stretchy='false'>)</mo></math> gravity framework where we have a conformal constant and an <italic>RT</italic>-mixing term apart from an R term. The RT-mixing term introduces non-minimal coupling between gravity and matter. We consider the exponential SUSY potential <math altimg='si2.svg'><mi>V</mi><mo stretchy='false'>(</mo><mi>&#981;</mi><mo stretchy='false'>)</mo><mo linebreak='goodbreak' linebreakstyle='after'>=</mo><msup><mrow><mi>M</mi></mrow><mrow><mn>4</mn></mrow></msup><mrow><mo stretchy='true'>(</mo><mn>1</mn><mo linebreak='badbreak' linebreakstyle='after'>&#8722;</mo><msup><mrow><mi>e</mi></mrow><mrow><mo linebreak='badbreak' linebreakstyle='after'>&#8722;</mo><mi>&#955;</mi><mi>&#981;</mi><mo stretchy='false'>/</mo><msub><mrow><mi>M</mi></mrow><mrow><mi>p</mi><mi>l</mi></mrow></msub></mrow></msup><mo stretchy='true'>)</mo></mrow></math> and a novel potential <math altimg='si3.svg'><mi>V</mi><mo stretchy='false'>(</mo><mi>&#981;</mi><mo stretchy='false'>)</mo><mo linebreak='goodbreak' linebreakstyle='after'>=</mo><mi>&#955;</mi><msubsup><mrow><mi>M</mi></mrow><mrow><mi>p</mi><mi>l</mi></mrow><mrow><mn>4</mn><mo linebreak='badbreak' linebreakstyle='after'>&#8722;</mo><mn>2</mn><mi>&#945;</mi></mrow></msubsup><msup><mrow><mi>&#981;</mi></mrow><mrow><mn>2</mn><mi>&#945;</mi></mrow></msup><msup><mrow><mi mathvariant='normal'>sin</mi></mrow><mrow><mn>2</mn></mrow></msup><mo>&#8289;</mo><mrow><mo stretchy='true'>(</mo><mfrac><mrow><mi>&#946;</mi><msubsup><mrow><mi>M</mi></mrow><mrow><mi>p</mi><mi>l</mi></mrow><mrow><mi>&#945;</mi></mrow></msubsup></mrow><mrow><msup><mrow><mi>&#981;</mi></mrow><mrow><mi>&#945;</mi></mrow></msup></mrow></mfrac><mo stretchy='true'>)</mo></mrow></math>. With the help of COBE normalization, we constrain values of different parameters and extract the field value at the time of Hubble crossing. The end of inflation is marked by <math altimg='si4.svg'><msub><mrow><mover accent='true'><mrow><mi>&#1013;</mi></mrow><mrow><mo stretchy='false'>&#732;</mo></mrow></mover></mrow><mrow><mi>v</mi></mrow></msub><mo stretchy='false'>(</mo><msub><mrow><mi>&#981;</mi></mrow><mrow><mi>i</mi></mrow></msub><mo stretchy='false'>)</mo><mo linebreak='goodbreak' linebreakstyle='after'>=</mo><mn>1</mn></math> where <math altimg='si5.svg'><msub><mrow><mi>&#981;</mi></mrow><mrow><mi>i</mi></mrow></msub></math> is the field value at the end of inflation. Equipped with these values, we then move on to calculate values of spectral index <math altimg='si6.svg'><msub><mrow><mi>n</mi></mrow><mrow><mi>s</mi></mrow></msub></math> and tensor-to-scalar ratio <italic>r</italic>. Our predicted values of <math altimg='si6.svg'><msub><mrow><mi>n</mi></mrow><mrow><mi>s</mi></mrow></msub></math> and <italic>r</italic> fall within their observed values from the Planck 2018 survey and BICEP/Keck array measurement for both potential, making them plausible candidates for the inflationary model. We also display the variation of the tensor-to-scalar ratio and spectral index with the coefficient of RT-mixing term for fixed values of e-fold number. There, we find the existence of two local maxima of <math altimg='si6.svg'><msub><mrow><mi>n</mi></mrow><mrow><mi>s</mi></mrow></msub></math>, which occur at a negative and a positive value of <italic>&#958;</italic>, the coefficient of <italic>RT</italic>-mixing term. Our analysis finds a significant impact of <italic>&#958;</italic> on values of observables.

Sohan Kumar Jha

Anisur Rahaman

Non-minimal <italic>RT</italic> coupling and its impact on inflationary evolution in <italic>f</italic>( <italic>R</italic>, <italic>T</italic>) gravity