arXiv subjects

Phongpichit Channuie

Publications and source records attributed to Phongpichit Channuie.

At least 19 recordsLinked to original sources

arXiv2026

Elastic toroidal vector dark matter through a dark photon in the LUX-ZEPLIN high recoil window

The 2026 LUX-ZEPLIN search reports one nuclear recoil candidate at $248\pm23_{\rm stat}\pm23_{\rm sys}~\mathrm{keV}$ in an extended window reaching about $270~\mathrm{keV}$. We consider elastic scattering of neutral complex vector dark matter through its dimension-six toroidal electromagnetic moment and find appreciable spectral weight in this recoil region. The nonrelativistic reduction correlates $\mathcal O_{17}$ and $\mathcal O_{20}$, relating a coherent charge branch to a transverse spin tensor branch. For $m_X=1~\mathrm{TeV}$, natural xenon exhibits a broad high recoil maximum at $204.8$ to $206.6~\mathrm{keV}$ and retains $80.4$ to $85.4\%$ of this maximum at $248~\mathrm{keV}$. Resolving the interaction through a dark photon relates the high-to-low recoil ratio to the mediator mass. A renormalizable $SU(2)_X\times U(1)_D$ realization stabilizes the complex vector by a residual $Z_3$ gauge symmetry and generates the toroidal current through vectorlike messengers carrying a physical CP phase. For a benchmark with $m_X=0.998~\mathrm{TeV}$ and $m_{A'}=0.450~\mathrm{GeV}$, $R(248)/R(50)=1.43$ for GCN and $1.21$ for JJ55, while the odd $A$ xenon fraction remains above $99.9\%$. The response level ratio between the $350$ to $590~\mathrm{keV}$ and $100$ to $270~\mathrm{keV}$ intervals is about $0.46$ at this benchmark. The tensor branch is absent for spin zero argon, whereas annual modulation remains at the few percent level. The resulting spectral, isotope, target, timing, mediator, and high energy dependences give correlated tests of an elastic tensor interpretation of the LZ recoil.

hep-ph↗

arXiv2026

Yukawa modification of Traversable Wormholes supported by Holographic Dark Energy

Inspired by holographic dark energy models, we extend the analysis performed in Ref.\cite{RGPC} taking into account Yukawa deformations on the different energy density (HDE) profiles. The profiles we have explored are: the Bekenstein-Hawking HDE, the Moradpour energy density, the Standard Renyi HDE and the Mixed Energy Density. With the help of an inhomogeneous Equation of State of the form $p_{r}(r)=ω_{r}\left( r\right) ρ(r)$, we have considered Zero Tidal Forces. Differently from the original case, only a particular case of the family of the Bekenstein-Hawking HDE profiles distorted by the Yukawa term has developed a divergent $ω_{r}\left( r\right) $ for $r\rightarrow \infty $. To cure such a divergence we have introduced a modification at large distances in order to have a finite result. This means that the Zero Tidal Forces can be imposed in a very large but limited region of the spacetime. Such modification did not change the behavior of the Equation of State close to the throat. For every proposal we have computed the components of the Stress-Energy Tensor. What we have found is that the Yukawa-Bekenstein-Hawking HDE is the only positive profile, while the Yukawa-Moradpour and the Yukawa-Renyi have a limited region where the energy density is positive. The remaining Yukawa-Mixed Energy Density is always negative. This means that the Yukawa distortion introduces a kind of negative energy density.

gr-qc↗

arXiv2026

Removability criterion for radiative corrections to the Starobinsky attractor in weakly nonlocal gravity

Radiative corrections at the percent level can shift the predictions of $α$-attractor and Starobinsky-like models into the region of the $(n_s,r)$ plane preferred by ACT DR6. We show that the decisive property is not the size of a correction but whether it is removable. In the slow-roll $N$-formalism the observables are functionals of $\eps(N)$, and equality of $\eps(N)$ on an interval reconstructs the potential up to an amplitude rescaling and a shift of the canonical field. A larger class, selected by $(V/V')Δ'={\rm const}$, preserves the leading predictions and provides a criterion for any proposed deformation. In weakly nonlocal completions of $R+R^{2}$ the improvement scale $μ=H(ϕ)$ makes the renormalization-group time one half of the logarithm of the tree potential, so the local one-loop flow passes the test and evolves the model onto the E-model family $V\propto(1-e^{-\sqrt{2/3}\,ϕ/\mpl})^{p}$ with $p=2+K$. Since the divergent local beta functions of these super-renormalizable completions are one-loop exact, no higher-loop local running modifies this picture. The induced shifts are $\ord(\ln N/N^{2})$ in $n_s$, obtained in closed form for the removable part and numerically for the rest. The number of $e$-folds, which the criterion does not protect, contributes at the \red{$22\%$} level with an opposite sign. Matter-induced corrections fail the same test at leading order, which is why they shift the predictions. Among the deformations proposed since ACT DR6, an $R^{n}$ term in $f(R)$ gives $(V/V')Δ'=\ord(N^{n-1})$, so only $n=2$ is removable, and no deformation that increases $n_s$ satisfies the criterion. For Standard Model matter, the removable channel is fixed by the Higgs nonminimal coupling alone and is $\ord(10^{-11})$, because the measured amplitude sets the coefficient of $R^{2}$ to $5.1\times10^{8}$.

gr-qc↗

arXiv2026

Probing scalarized wormholes through quasi-periodic oscillations and spinning particle dynamics

We investigate the dynamics of test particles in a three-parameter scalarized wormhole spacetime within Einstein-scalar field theory. For spinless particles, we derive the orbital and epicyclic frequencies and compute twin-peak QPO spectra using the ER3 and ER4 resonance models. The scalar coupling parameter $g_s$ shifts the innermost stable circular orbit to larger radii and systematically modifies the characteristic 3:2 resonance condition. Extending to spinning particles via the Mathisson-Papapetrou-Dixon formalism, we find that spin-curvature coupling significantly alters the effective potential and innermost stable circular orbit parameters. The maximum physically admissible spin increases monotonically with the scalar coupling. Analysis of particle collisions near the wormhole throat reveals that both scalar coupling and relative spin orientation determine collision energetics, with anti-aligned spin configurations producing substantially higher energies. Our results suggest that the combined effects of scalar coupling and spin-curvature interaction leave distinct imprints on QPO frequencies and collision processes, potentially providing observable signatures for distinguishing scalarized wormholes from standard black holes.

gr-qc↗

arXiv2026

Coherent and Stochastic Axion Dark Matter from Thermal Relaxation

An axion driven toward a thermal minimum need not remain a coherent condensate. We derive the coupled attenuation of the field mean and production of stochastic momentum modes in an expanding plasma. A single momentum dependent optical depth partitions every mode between coherent power and Bose occupation, placing standard misalignment, partial relaxation, and stochastic production in one dynamical relation. Finite spatial and temporal response suppresses high momentum production, so the stochastic relic has lower mean momentum and a shorter free streaming length than an equilibrium population at fixed mass and bath temperature. A weakly coupled realization produces the dark matter abundance, reduces inherited coherent isocurvature, and confines production correlations to scales removed by collisionless propagation. Thermal relaxation therefore determines the composition, momentum distribution, and transported structure of axion dark matter.

hep-ph↗

arXiv2026

Higher-order generalized uncertainty principle corrections to Casimir-supported traversable wormholes

We investigate traversable wormholes supported by Casimir vacuum energy with second-order generalized uncertainty principle (GUP) corrections. For two representative GUP models, we derive higher-order corrections to the Casimir energy and construct exact wormhole solutions in general relativity. The resulting geometries satisfy the throat, flare-out, and asymptotic-flatness conditions. Higher-order corrections modify the wormhole mass and reduce the exotic matter required, although the null and weak energy conditions remain violated near the throat. We further analyze weak gravitational lensing and gravitational-wave echoes, finding model-dependent signatures that may distinguish different GUP realizations. By relating the dimensionless parameter used in the solutions to the conventional phenomenological GUP parameter, we show that its physical interpretation depends strongly on the throat radius. Most current experimental bounds favor near-Planckian throats for appreciable GUP corrections, while macroscopic throats generally require much weaker corrections. These results provide a framework for confronting GUP-corrected Casimir wormholes with laboratory constraints and astrophysical observations.

gr-qc↗

arXiv2026

Noncommutative black holes: Topological bulk-boundary correspondence and Binary Merger Bounds

We investigate the thermodynamic topology of charged AdS black holes in a non-commutative spacetime sourced by Lorentzian-smeared matter distributions. Since exact analytical solutions for the critical thermodynamic quantities are not available, we employ a perturbative expansion in the non-commutative parameter and validate the resulting expressions through numerical analysis. Using the generalized off-shell free-energy framework, we explore the topological structure of the thermodynamic phase space and evaluate the corresponding winding number that characterizes the phase transitions. Our results reveal that non-commutative effects introduce qualitative modifications to the thermodynamic behavior compared with the standard Reissner-Nordström AdS black hole. Furthermore, we demonstrate that the bulk and boundary descriptions possess an identical global thermodynamic topology, providing strong evidence for the correspondence between their topological structures. We also investigate the lower bound on the remnant mass implied by the second law of black-hole thermodynamics and observe that non-commutative corrections modify key thermodynamic quantities, with particular emphasis on the entropy and the final black-hole mass.

gr-qc↗

arXiv2026

Testing the Direction of Dark Sector Interaction Using Late-Time Datasets

In this work, we constrain the phenomenological interacting dark energy $ξ$IDE model using baryon acoustic oscillation measurements from DESI Data Release 1 and Data Release 2, combined with cosmic chronometer measurements, compressed CMB likelihoods, and three different Type Ia supernova compilations: Pantheon$^+$, DES-Dovekie, and Union3. We constrain the parameters of the $ξ$IDE model using a Markov Chain Monte Carlo analysis, using the nested sampling algorithm implemented in the \texttt{dynesty} package through the cosmological inference code \texttt{SimpleMC}. Compared to $Λ$CDM, the $ξ$IDE model favors slightly higher values of the Hubble constant, leading to a reduction in the Hubble tension. However, the tension is not completely resolved for any dataset combination. The parameter $ξ$ is consistently constrained to values close to its $Λ$CDM prediction, indicating no statistically significant deviation from the standard cosmological scenario. Similarly, except for the CMB + DESI DR1 + CC dataset combination, the dark energy equation-of-state parameter prefers values of $w_{\rm X}>-1$, showing a preference for quintessence-like behavior and providing evidence for dynamical dark energy. The interaction parameter combination, $ξ+3w_{\rm X}$, is found to be negative for all dataset combinations, corresponding to energy transfer from dark energy to dark matter. The strongest preference is obtained for the CMB + DESI DR2 + CC + Union3 dataset combination, yielding $ξ+3w_{\rm X}=-0.035\pm0.023$, which corresponds to a deviation of only $1.52σ$ from the non-interacting limit. Therefore, the current data provide only a weak indication of a non-zero dark-sector interaction. Model comparison based on the $Nσ$ statistic shows weak evidence in favor of the interacting scenario, while Bayesian evidence consistently prefers the $Λ$CDM model.

astro-ph.CO↗

arXiv2026

Transient Dynamical Wormholes with Decaying Radial Energy Flux

We investigate a class of time-dependent traversable wormholes within the framework of general relativity by allowing the shape function to vary with time. In this setting, the evolution of the geometry is directly connected to a radial energy flux through the off-diagonal component of the Einstein field equations, providing a natural mechanism for non-static configurations. We obtain exact solutions in which the geometry consists of a static background supplemented by a transient term that diminishes with time. The resulting spacetime satisfies the standard conditions required for a traversable wormhole, including the presence of a throat, the flaring-out condition, and asymptotic flatness. An analysis of the energy conditions indicates that the null energy condition is violated in the vicinity of the throat, although the degree of violation decreases as the system evolves. This feature is examined further through a volume integral that measures the total amount of exotic matter, demonstrating that it approaches a constant value at late times. We also study the response of the system to small perturbations and find that, for a suitable choice of parameters, the configuration remains stable with perturbations decaying over time. We discuss how this flux-driven mechanism relates to the alternative and extensively studied approach in which wormhole evolution is instead carried by a cosmological scale factor, and we identify possible physical origins of the assumed radial flux in terms of null-fluid matter sources. Overall, the model describes a wormhole spacetime whose evolution is controlled by energy transport, leading to a gradual transition toward a static configuration. This framework offers a simple and physically motivated approach to dynamical wormholes and may be useful for exploring more realistic scenarios in both general relativity and extended theories of gravity.

gr-qc↗

arXiv2026

Analytical Solutions to the Wheeler-DeWitt Equation in Rosen-Lagrangian Cosmology via the Eisenhart Lift

The Rosen Lagrangian framework promotes the cosmological constant to a scale-factor-dependent quantity, $Λ(a)=Λ_{0}a^λ$, thereby providing a dynamical dark energy scenario for $λ\neq 0$. In the special case $λ=0$, the model naturally reduces to the standard $Λ$CDM cosmology. Within this framework, the conformal Killing equations are employed to determine the conformal factor $\mathcal{F}(a)$, which is expressed in terms of the effective potential $V_{\rm eff}$ and its derivative $V'_{\rm eff}$. Furthermore, the Eisenhart lift formalism introduces an additional field $χ$, allowing the cosmological dynamics to be reformulated through a purely kinetic lifted action. This geometrical construction provides a powerful approach to quantum cosmology by transforming the Wheeler-DeWitt equation into a tractable form that admits analytic solutions. Such solutions are particularly relevant in cosmological epochs dominated by the cosmological constant, including both the inflationary era of the early Universe and the late-time accelerated expansion. Consequently, this framework offers a promising avenue for connecting geometrical methods, quantum cosmology, and dynamical dark energy within a unified description.

gr-qc↗

arXiv2026

Revisiting Thermodynamics of the Hayward Black Holes and Exploring Binary Merger Bounds

In this article, we revisit the thermodynamics of Hayward black holes [1] in asymptotic flat spacetime and obtain the bounds on the final mass post merger after head-on collision event of two equal mass black holes. We revisit thermal properties of these black holes from a perspective that the laws of black hole thermodynamics remain valid. Under this condition a novel entropy formula appears naturally with a logarithmic correction term along with one extra term. We discuss phase structure of the black holes. Next, we obtain the bounds on the final black hole mass parameter using the validity of the second law of black hole thermodynamics with the new entropy formula. We discuss the impact of the Hayward parameter on thermal and merger properties of these black holes.

gr-qc↗

arXiv2026

Simpson-Visser-AdS Black Holes: Thermodynamics and Binary Merger

In this article, we performed Simpson-Visser (SV)-regularization scheme to Anti-de Sitter (AdS) black holes and then studied thermal properties of the resulting spacetime geometry. We considered the validity of the first law of black hole thermodynamics in this case and derived an entropy formula consistent with this new regular geometry. Next, we carried out the free energy analysis and studied the phase structure of these black holes. We discovered non-trivial phase transition properties dependent on the SV-regularization parameter. We also considered the validity of the second law of black hole thermodynamics and analyzed a merger scenario of two equal mass SV-regular black holes. In particular, we investigated the impact of the SV-regularization parameter on the constraints on post-merger black hole mass. Intrestingly, we found that the bounds initially increase and then fall sharply with increasing the SV-regularization parameter. All results are compared with standard black holes for vanishing SV-regularization parameter.

gr-qc↗

arXiv2026

Rényi Law Constraints on Gauß-Bonnet Black Hole Merger

In this article, we explore the Rényi law constraints on black hole merger in Gauß-Bonnet (GB) gravity. Specifically, we consider the case of static solutions in five-dimensional (5D) Anti-de-Sitter (AdS) spacetime and study the constraints on merger of two equal mass black holes. We calculate the general Rényi entropy expression and utilize it to study the bounds on the final black hole mass post-merger. We study its variation with the Rényi parameter. We also compare the results with those for black holes in General Relativity (GR). We find that the GB term has a significant impact on the bounds for black hole merger. The bounds for GB gravity become weaker for the zeroth order Rényi entropy and stronger for higher order Rényi entropies in comparison to GR.

gr-qc↗

arXiv2026

Constraining $β$-Exponential Inflation with the latest ACT observations

Recent observations from the Atacama Cosmology Telescope (ACT), especially when combined with DESI baryon acoustic oscillation data, indicate a scalar spectral index $n_s$ higher than the value reported by \textit{Planck} 2018, placing tension on universal inflationary attractor models. Motivated by this discrepancy, we investigate the inflationary predictions of the $β$-exponential potential, $V(ϕ)=V_0\left(1-λβϕ/M_p\right)^{1/β}$ considering both minimally and non-minimally coupled realizations. This potential generalizes standard exponential inflation and naturally arises in braneworld scenarios. We derive analytical expressions for the slow-roll parameters and inflationary observables using a perturbative expansion in the non-minimal coupling $ξ$, and validate these results through numerical calculations. In the minimally coupled case, the model predicts $n_s \simeq 0.976$ and $r \simeq 0.035$ for $N=50$ and moderate values of β, remaining compatible with ACT+DESI constraints at the 1σlevel while yielding a spectral tilt larger than the universal attractor prediction. Introducing a small non-minimal coupling significantly improves agreement with observations by suppressing the tensor-to-scalar ratio while preserving the enhanced scalar tilt. For $N=60, λ\sim 0.3-0.5$, and $β\sim O(1-5)$, the non-minimally coupled model yields $n_s \simeq 0.974-0.976$ and $r \lesssim 0.03$, comfortably consistent with ACT, DESI, and BICEP/Keck bounds. Our results show that the $β$-exponential potential, especially when implemented with a non-minimal coupling, exhibits good agreement with the latest CMB observations. Our inflationary predictions of the non-minimal model of $n_s$ and $r$ confirming the leading-order contributions in $ξ$ are sufficient to capture the essential features of both $r$ and $n_s$ in observationally relevant regimes.

gr-qc↗

arXiv2025

Constraining non-minimally coupled squared-Quartic Hilltop Inflation in light of ACT observations

The combination of the data from the Dark Energy Spectroscopic Instrument (DESI) with the recent measurements from the Atacama Cosmology Telescope (ACT) indicate that the scalar spectral index $ n_s $ has a larger value than the Planck 2018 which leads to tension within standard inflationary models. In this study in order to explain the new data, We consider the squared-Quartic Hilltop inflation potential $ V(ϕ) = V_0 [1 - λ(ϕ/M_p)^4]^2 $ within the Einstein and Jordan frames. In the Jordan frame we introduce the coupling term $ ξϕ^2 R $ and we calculate analytic expressions for the slow-roll parameters, scalar spectral index, and tensor-to-scalar ratio on the weak and strong coupling regimes. In the weak limit ($ ξ\ll 1 $), perturbative corrections slightly increase $ n_s $ and suppress $ r $, leading to $ n_s \simeq 0.9743 $ and $ r \sim 7.8 \times 10^{-5} $ for representative parameters $ λ= 10^{-3}, ξ= 10^{-3}, {\cal N} = 117 $, values which are in agreement with the joint Planck--ACT--DESI (P-ACT-LB) constraints. On the other hand, for a strong coupled ($ ξ\gg 1 $), the conformal rescaling provides an exponentially flat potential plateau, which allows us to calculate $ n_s \approx 0.9743 $ with $ r \lesssim 5 \times 10^{-4} $ for $ {\cal N} = 65{-}70 $, consistent with ACT and BK18 bounds. The associated energy scale of inflation, $ V_0^{1/4} \sim 10^{-3}{-}10^{-2} M_p $, remains compatible with high-scale inflationary scenarios.

astro-ph.CO↗

arXiv2025

Radiative-Corrected Higgs Inflation in Light of the Latest ACT Observations

Recent measurements from the Atacama Cosmology Telescope (ACT), particularly when combined with DESI baryon acoustic oscillation data, have reported a scalar spectral index $n_s$ slightly higher than that inferred by {\it Planck}~2018, suggesting a mild tension with the predictions of standard inflationary attractor models. In this work, we revisit the quantum-corrected Higgs inflation scenario within the framework of a non-minimally coupled scalar field theory. Starting from the one-loop effective action, we incorporate radiative corrections through the anomalous scaling parameter ${\bf A_I}$ and derive analytic expressions for the inflationary observables $n_s$ and $r$ in the Einstein frame. Our analysis demonstrates that quantum corrections naturally shift $n_s$ toward higher values while keeping the tensor-to-scalar ratio $r$ suppressed. For ${\cal N} = 60$, the model predicts $n_s \simeq 0.9743$ and $r \simeq 5.4\times10^{-3}$, in excellent agreement with the latest ACT+DESI (P-ACT-LB) data and fully consistent with the \textit{Planck}~2018 limit $r < 0.036$. The derived constraint $4.36\times10^{-10} < λ/ξ^{2} < 10.77\times10^{-10}$ confirms the robustness of the quantum-corrected Higgs framework and indicates that near-future CMB polarization experiments such as CORE, AliCPT, LiteBIRD, and CMB-S4 will be able to probe the predicted parameter space with high precision.

astro-ph.CO↗

arXiv2025

ACT Constraints on Marginally Deformed Starobinsky Inflation

We investigate the inflationary phenomenology of a marginally deformed Starobinsky model, motivated by quantum corrections to the $R^{2}$ term, in light of the latest cosmological observations. In this framework, the inflationary potential acquires a small deformation parameter, $γ$, which shifts predictions away from the exact Starobinsky limit. Using the slow-roll formalism, we derive analytic expressions for the spectral index $n_{s}$ and tensor-to-scalar ratio $r$ and confront them with constraints from Planck, ACT, and DESI data. Our analysis shows that nonzero values of $γ$ raise both $n_{s}$ and $r$, thereby alleviating the $\gtrsim 2σ$ tension between the Starobinsky $R^{2}$ scenario and the ACT+DESI (P-ACT-LB) measurements, which favor $n_{s} \simeq 0.9743 \pm 0.0034$. For $N \sim 60$ $e$-foldings, the model consistently reproduces the observed amplitude of primordial perturbations while predicting tensor contributions within current observational bounds. We also demonstrate that the deformation softens the otherwise severe fine-tuning of the quartic self-coupling in minimally coupled inflation. The parameter range $γ\sim \mathcal{O}(10^{-3})$-$\mathcal{O}(10^{-2})$ emerges as phenomenologically viable, providing a natural extension of Starobinsky inflation compatible with present data. We conclude that marginally deformed $R^{2}$ inflation remains a compelling and testable candidate for the primordial dynamics of the Universe, with future CMB and gravitational-wave observations expected to further probe its parameter space.

gr-qc↗

arXiv2025

Traversable Wormholes in non-minimal Einstein-Yang-Mills Gravity: Geometry, Energy Conditions, and Gravitational Lensing

This work presents a new class of static, spherically symmetric traversable wormhole solutions within the framework of non-minimal Einstein-Yang-Mills (EYM) gravity, where the SU(2) Yang-Mills field is purely magnetic. By adopting a constant redshift function and introducing a direct coupling between the Ricci scalar and the Yang-Mills field strength, we investigate the role of the non-minimal coupling constant $ξ$ and the magnetic charge $Q$ in shaping the wormhole geometry. Our analysis shows that for small values of $ξ$, the flare-out and throat conditions can be satisfied, allowing physically viable traversable wormholes without requiring externally introduced exotic matter. The Arnowitt-Deser-Misner (ADM) mass is evaluated, revealing that for $ξ< 0.01$ it grows monotonically with charge, whereas for $ξ\gtrsim 0.01$ it decreases with increasing charge, signaling a reduction in the total mass-energy of the system. An examination of the energy conditions indicates localized violations of the null and weak energy conditions at the throat, while the strong energy condition remains satisfied. Finally, the study of gravitational lensing confirms that the deflection angle of light is consistently positive, reflecting the overall attractive nature of the wormhole gravitational field. These results highlight the significant role of non-minimal gauge-gravity couplings in enabling traversable wormholes with distinct observational signatures.

gr-qc↗