Phongpichit Channuie

Phongpichit Channuie

Walailak University
*This is an algorithmically generated author record based on publicly available information.
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Phongpichit Channuie has a total of 149 co-authors. Here are the top co-authors by number of shared publications:

Latest Publications

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    Testing the direction of dark sector interaction using late-time datasets

    by Anil Kandel, Phongpichit Channuie, Ertan Güdekli, Farruh Atamurotov

    We constrain the phenomenological interacting dark energy ( $$\xi $$ ξ IDE) model, in which the relative evolution of dark matter and dark energy is characterized by the scaling relation $$\rho _\textrm{X}/\rho _m \propto a^{\xi }$$ ρ X / ρ m ∝ a ξ , using baryon acoustic oscillation measurements from DESI Data Releases 1 and 2, combined with cosmic chronometers, compressed CMB likelihoods, and the Pantheon $$^+$$ + , DES-Dovekie, and Union3 Type Ia supernova samples. Parameter constraints are obtained using the cosmological inference code . Relative to $$\Lambda $$ Λ CDM, the $$\xi $$ ξ IDE model mildly favors higher values of the Hubble constant, reducing but not resolving the $$H_0$$ H 0 tension. The parameter $$\xi $$ ξ remains close to its $$\Lambda $$ Λ CDM limit, while most dataset combinations favor $$w_\textrm{X}>-1$$ w X > - 1 , indicating a mild preference for quintessence-like dark energy. The interaction combination $$\xi +3w_\textrm{X}$$ ξ + 3 w X is negative for all dataset combinations, corresponding to energy transfer from dark energy to dark matter. The strongest deviation from the non-interacting limit is obtained for CMB + DESI DR2 + CC + Union3, with $$\xi +3w_\textrm{X}=-0.035\pm 0.023$$ ξ + 3 w X = - 0.035 ± 0.023 , corresponding to only $$1.52\sigma $$ 1.52 σ . Although the $$N\sigma $$ N σ statistic shows a weak preference for the interacting scenario, Bayesian evidence consistently favors $$\Lambda $$ Λ CDM. Overall, observations provide no compelling evidence for a nonzero dark-sector interaction, despite a consistent mild preference for energy transfer from dark energy to dark matter.

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    Bulk-viscous five-dimensional Kaluza–Klein cosmology within non-conservative gravitational frameworks and its implications for early-universe dynamics

    by Phongpichit Channuie, Shahid Iqbal, Muhammad Ramzan, Muhammad Irfan, Imtiaz Khan, Chengxun Yuan

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    Transient dynamical wormholes with decaying radial energy flux

    by Allah Ditta, Phongpichit Channuie

    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. By adopting a decaying flux profile, 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. The corresponding matter content is determined explicitly and shows a clear temporal evolution governed by the decay parameter. 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.

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    Revisiting the evidence for dynamical dark energy: from DES-SN5Y to DES-Dovekie

    by Anil Kandel, Farruh Atamurotov, Ertan Güdekli, Phongpichit Channuie, Gulzoda Rakhimova

    Recent analyses combining DESI DR2 BAO measurements with CMB and supernova data have suggested a preference for dynamical dark energy, particularly when using the DES-SN5Y and DES-SN5Y $$(z>0.1)$$ ( z > 0.1 ) supernova samples. With the revision of this dataset into the DES-Dovekie compilation, it is important to reassess the robustness of this result. In this work, we analyze a broad class of dark energy parametrizations, including w CDM, $$w_0w_a$$ w 0 w a CDM, BA, JBP, Efstathiou, and GEDE models, using DESI DR2 BAO, a compressed CMB likelihood, and supernova data. We find that the DES-SN5Y dataset consistently yields a stronger preference for deviations from $$\Lambda $$ Λ CDM compared to DES-Dovekie. In particular, redshift-dependent parametrizations favor the region $$w_0 > -1$$ w 0 > - 1 and $$w_a < 0$$ w a < 0 , corresponding to a Quintom-B–type evolution with phantom crossing. This behavior is observed across multiple models, indicating that it is not specific to a single parametrization. We find that the DES-SN5Y $$(z>0.1)$$ ( z > 0.1 ) sample also preserves the same qualitative behavior, although the deviations from the $$\Lambda $$ Λ CDM limit become significantly weaker compared to the full DES-SN5Y sample. However, when DES-Dovekie is used, the statistical preference for dynamical dark energy is significantly reduced. The improvement over $$\Lambda $$ Λ CDM drops to below the $$1\sigma $$ 1 σ level for most models, and the Bayesian evidence weakens from moderate to weak or inconclusive. Similarly, for the DES-SN5Y $$(z>0.1)$$ ( z > 0.1 ) sample, the preference for dynamical dark energy becomes intermediate between the DES-SN5Y and DES-Dovekie cases, with mostly weak or inconclusive evidence. Overall, the DES-Dovekie and DES-SN5Y $$(z>0.1)$$ ( z > 0.1 ) datasets weaken the preference for dynamical dark energy compared to the full DES-SN5Y dataset.

    Cited by 3
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    Enhancing Engineering Students' Understanding of Fluid Flow Using Motion Analysis Software: A Lab@Home‐Inspired Contemporary Physics Laboratory

    by Thammarong Eadkhong, Phongpichit Channuie, Nirundorn Matan, Punsiri Dam‐O

    An experimental toolset for efflux‐speed measurement was developed by refining a prototype originally implemented during the COVID‐19 pandemic. A fluid mechanics experiment—the Speed of Efflux Analysis Laboratory—was designed for first‐year engineering students to introduce fundamental fluid dynamics concepts. Tracker video analysis software was integrated to enhance students' digital literacy and support data analysis. The study involved 430 students and a 6‐student focus group. Prior knowledge, learning objectives, suitable apparatus, and curricular alignment were systematically considered in the design process. The experimental setup produced data consistent with theoretical predictions, enabling students to apply the continuity equation and Bernoulli's principle to real measurements. Post‐test scores demonstrated improved understanding, and students effectively used Tracker software to analyze fluid motion. This experiment can be implemented in introductory physics labs to promote conceptual understanding, develop digital literacy, reduce equipment costs, and support flexible lab‐at‐home learning, while enhancing interdisciplinary STEM skills across physics and engineering contexts.

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    Rényi law constraints on Gauß–Bonnet black hole merger

    by Neeraj Kumar, Ankur Srivastav, Phongpichit Channuie

    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.

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    Constraining non-minimally coupled squared-quartic hilltop inflation in light of ACT observations

    by Jureeporn Yuennan, Thammarong Eadkhong, Farruh Atamurotov, Phongpichit Channuie

    Cited by 7
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    Constraining $\beta $-exponential inflation with the latest ACT observations

    by Jureeporn Yuennan, Farruh Atamurotov, Salvatore Capozziello, Phongpichit Channuie

    Recent observations from the Atacama Cosmology Telescope (ACT), especially when combined with DESI baryon acoustic oscillation data, indicate a scalar spectral index $$ n_s $$ n s higher than the value reported by Planck 2018, placing tension on universal inflationary attractor models. Motivated by this discrepancy, we investigate the inflationary predictions of the $$\beta $$ β -exponential potential, $$ V(\phi )=V_0\left( 1-\lambda \beta \phi /M_p\right) ^{1/\beta }$$ V ( ϕ ) = V 0 1 - λ β ϕ / M p 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 $$\xi $$ ξ , and validate these results through numerical calculations. In the minimally coupled case, the model predicts $$ n_s \simeq 0.976 $$ n s ≃ 0.976 and $$ r \simeq 0.035 $$ r ≃ 0.035 for $$N=50$$ N = 50 and moderate values of $$\beta $$ β , remaining compatible with ACT+DESI (P-ACT-LB) constraints at the $$1\sigma $$ 1 σ level 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 $$N=60 $$ N = 60 , $$ \lambda \sim 0.3\!-\!0.5 $$ λ ∼ 0.3 - 0.5 , and $$ \beta \sim \mathcal {O}(1\!-\!5) $$ β ∼ O ( 1 - 5 ) , the non-minimally coupled model yields $$ n_s \simeq 0.974\!-\!0.976 $$ n s ≃ 0.974 - 0.976 and $$ r \lesssim 0.03 $$ r ≲ 0.03 , comfortably consistent with ACT, DESI, and BICEP/Keck bounds. Our results show that the $$\beta $$ 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 $$n_s$$ n s and r confirming the leading-order contributions in $$\xi $$ ξ are sufficient to capture the essential features of both r and $$n_s$$ n s in observationally relevant regimes.

    Cited by 5
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    Constraining $β$-Exponential Inflation with the latest ACT observations

    by Jureeporn Yuennan, Farruh Atamurotov, Salvatore Capozziello, Phongpichit Channuie

    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.

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    Dynamics of spinning particles around the loop quantum black hole

    by Gulnisa Abdukayumova, Farruh Atamurotov, Ahmadjon Abdujabbarov, Phongpichit Channuie, G. Mustafa

    Cited by 4
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