arXiv subjects

Chakrit Pongkitivanichkul

Publications and source records attributed to Chakrit Pongkitivanichkul.

At least 19 recordsLinked to original sources

arXiv2026

Relocating the SIMP Miracle in the Axion Portal

In the strongly interacting massive particle (SIMP) scenario, dark matter is a pseudo-Nambu--Goldstone boson whose abundance is set by a three-to-two Wess--Zumino--Witten process. We study this scenario in an axion portal and find that the kinetic contact the canonical mechanism assumes is excluded by bounds on sub-GeV axion-like particles (ALPs). The dark sector then freezes out at its own temperature, so the relic abundance no longer fixes the self-interaction cross section but predicts the portal coupling instead. Moreover, the portal operator is Hermitian and even in the ALP field, so no trilinear ALP--pion coupling arises. The contact term then drives $ππ\to aa$ with nothing to cancel against it, and we find the conversion four orders of magnitude faster than a trilinear estimate gives. This disfavours the minimal realisation in which the dark condensate alone generates the ALP mass. The realisation that survives instead makes the ALP slightly heavier than the dark pion. Matching the observed abundance then fixes the flavon vacuum expectation value at $V_ϕ\simeq 1.1\times10^{10} \ {\rm GeV}$ and leaves the dark scale open over more than an order of magnitude. The decay $K^+\toπ^+a$ requires the flavon to charge the leptons alone. The model then predicts a dark matter self-interaction of $0.20\,{\rm cm^2/g}$ at a dark pion mass of $140\ {\rm MeV}$, in a window running from $82$ to $169 \ {\rm MeV}$. The predictive power of the SIMP framework is therefore not lost but relocated, from the self-interaction to the flavon scale.

hep-ph↗

arXiv2026

A Thermodynamic Positivity Bound on Higher-Derivative 3-Form Couplings in de Sitter, and its Inflationary Consequences

We investigate the interplay between the thermodynamic positivity bounds and slow-roll inflation within a framework governed by a 3-form gauge field. Starting from classical considerations, we derive an upper bound on the mass of black holes in dS spacetime which constrains the admissible parameter space. To incorporate quantum gravity effects, we introduce higher-derivative corrections to the 3-form action and, by requiring the Wald entropy correction to be positive, obtain a strict bound on these terms. Evaluating the backreaction within a quasi-local thermodynamic cavity bounded by the zero-force surface, we find that the correction to the extremal mass vanishes, so that the exact Nariai state saturates the classical bound rather than being shifted below it. The resulting bound is found to be invariant under field redefinitions of the metric. Extending this setup to cosmological inflation, we examine the scalar dual of the 3-form in both large-field and small-field regimes. In the large-field limit, the potential acquires a Higgs-like structure that supports slow-roll inflation consistent with Planck data. In contrast, the small-field limit leads to an effective potential with an AdS minimum, rendering it inconsistent with the dS swampland constraints. Notably, we find that thermodynamic consistency can impose constraints more stringent than those derived from inflationary dynamics alone. These results underscore the utility of swampland-inspired principles in shaping viable models of early universe cosmology.

gr-qc↗

arXiv2026

Effect of Cosmic Neutrino Background on the Dark Matter Self-interaction via Neutrino force

Neutrino-pair exchange induces a neutrino force that can drive dark matter (DM) self-interactions and impact small-scale structure formation. In the presence of the cosmic neutrino background (C$ν$B), this force can be modified, with important consequences for DM phenomenology. We study the effect of the C$ν$B on neutrino forces, generated by the scalar and pseudoscalar interactions. We explore the significance of the background neutrino force on the scalar DM-neutrino portal model, including DM self-scattering and annihilation. Our results show that the interplay between attractive vacuum potential and repulsive background potential leads to a screening effect that varies across DM mass ($m_χ$) regimes, strongly affecting DM self-scattering in the DM mass $m_ν\lesssim m_χ\lesssim T_{C νB}$. Meanwhile, for DM annihilation, the screening completely vanishes the Sommerfeld Enhancement induced by the neutrino force. Overall, the C$ν$B substantially reshapes the viable coupling range for DM self-interactions while remaining compatible with current constraints, offering a pathway to small-scale structure problems.

hep-ph↗

arXiv2026

Odderon Form Factors in Reggeized Spin-2 Pomeron and Spin-3 Odderon Exchange in $pp$ and $p\bar p$ Elastic Scattering

We investigate the form-factor dependence of Reggeized tensor Pomeron and Odderon exchanges in high-energy elastic $pp$ and $p\bar p$ scattering. The spin structure is implemented through explicit covariant spin-2 and spin-3 projectors, kept factorized from the Reggeized scalar kernels, so that vertex effects can be separated from trajectory dynamics. Seven Odderon--proton form-factor parametrizations are tested against a global dataset including TOTEM $pp$ data at $\sqrt{s}=2.76$, $7$, $8$, and $13$~TeV and Tevatron $p\bar p$ data at $\sqrt{s}=1.80$ and $1.96$~TeV. A clear hierarchy is found. Six dipole, polynomial, Gaussian, and hybrid parametrizations give comparable fit qualities, $χ^2_{\rm red}\simeq 1.44$--$1.48$, whereas a one-parameter exponential form, $F_{\mathbb O}(t)=\exp[-B|t|/2]$, yields $χ^2_{\rm red}=0.98$ for 138 degrees of freedom. The fitted couplings and Regge slopes remain comparatively stable across the form-factor choices, indicating that the improvement is driven mainly by the Odderon--proton vertex rather than by large compensating shifts in trajectory parameters. The exponential form admits an impact-parameter interpretation as a Gaussian transverse profile, with an effective radius $\sqrt{\langle b^2\rangle}=\sqrt{2B}\,\hbar c$. The extracted radii are of hadronic size and suggest a peripheral soft Odderon interaction. The shrinking $t$-range over which the single-Regge-exchange description remains accurate at increasing energy indicates the onset of absorptive and unitarity corrections. These results provide a compact phenomenological framework for connecting the $pp/p\bar p$ dip--bump difference with the transverse structure of $C$-odd color-singlet exchange.

hep-ph↗

arXiv2026

Constraining Axion-Like Particle mediated Dark Matter with Observational Constraints: A Statistical and Machine Learning Approach

We present a comprehensive study of axion-like particle (ALP) mediated dark matter (DM) effects on neutron star (NS) structure within a relativistic mean-field framework with non-linear mesonic interactions constrained by nuclear and astrophysical data. We explore DM masses $m_χ\in [0,1000]\,\mathrm{GeV}$ and Fermi momenta $q_f \in [0,0.06]\,\mathrm{GeV}$, generating over 30{,}000 equations of state using two representative hadronic models, a stiff EoS (EoS1) and a soft EoS (EoS18), including a consistent crust description. A multi-level statistical filtering scheme based on voting, likelihood, and kernel density estimation is applied using constraints from radio and X-ray pulsars, GW170817, and the low-mass compact object HESS~J1731$-$347. We find that models satisfying the PSR~J0614$-$3329 radius constraint automatically comply with the HESS bound, allowing ALP-mediated DM to explain low-mass compact objects while remaining consistent with $2\,M_\odot$ NSs. For the stiff EoS, we obtain a lower bound $m_χ\gtrsim 43\,\mathrm{GeV}$, with preferred values $q_f = 0.034^{+0.020}_{-0.012}$ and $m_χ\in [101,949]\,\mathrm{GeV}$, while the soft EoS yields no strict lower bound, though large $m_χ$ and $q_f$ are disfavored. We also develop a supervised interpolation model using \texttt{AutoGluon} to infer DM parameters from NS mass--radius curves, achieving $R^2>0.998$, and show that $m_χ$ is mainly constrained by global radius ratios, whereas $q_f$ is driven by the tidal deformability $Λ_{1.4}$.

astro-ph.HE↗

arXiv2025

Axion-Like Particle Mediated Dark Matter and Neutron Star Properties in the QHD Model

We investigate the effects of the ALP-mediated dark matter (DM) model on neutron star properties using the Quantum Hadrodynamics model (QHD). Using the relativistic mean-field approximation with the QHD-ALP-DM framework, we compute the equation of state (EoS) of neutron stars. Based on our previous study, we find that typical ALP parameter values have no significant effect on the EoS. We then explore various parametrizations of this model by varying the DM Fermi momentum, $q_f$, and DM mass, $m_χ$. Our results show that increasing $q_f$ or $m_χ$ shifts the energy density to higher values while reducing the maximum mass, radius, and tidal deformability of neutron stars. Finally, comparison with observational constraints from gravitational wave events and pulsar measurements indicates that the allowed parameter space for this model is constrained to $q_f < 0.05$ GeV and $m_χ < 1000$ GeV. As a result, our study highlights the importance of next-generation gamma-ray observatories, such as the Cherenkov Telescope Array (CTA), in probing the ALP-mediated DM model.

astro-ph.HE↗

arXiv2025

Kaluza-Klein inspired a model of the inflation with the inversed power law potential in Bianchi type-I universe

This work considers the dynamics of the gauge vector and inflaton (dilaton) fields inspired by Kaluza-Klein theory in an inflationary universe with Bianchi type-I spacetime. The inverse power-law potential of the inflaton field is used to study dynamical system analysis. As a result, all fixed points in the autonomous system are non-hyperbolic fixed points, and one cannot determine their stability. Therefore, a center manifold theory is required to analyze the stability of the dynamical system properly. Interestingly, we found an isotropic attractor point which means that the universe undergoes accelerated expansion (inflation) from an anisotropic phase to an isotropic phase of the universe. According to the dynamical system analysis of the anisotropic Bianchi type-I universe with the inspired Kaluza-Klein model, our results supported the isotropization of the observed universe.

gr-qc↗

arXiv2025

Inverse Seesaw Mechanism and Axion Portal Fermionic Dark Matter

We propose a minimal extension of the Standard Model (SM) that addresses both the smallness of neutrino masses and the dark matter (DM) puzzle via the inverse seesaw mechanism and an axion portal fermionic DM. This model generates light neutrino masses without requiring high energy scales, enhancing its testability in future collider experiments. An axion-like particle (ALP) connects the SM and DM sectors, yielding a distinct phenomenology. Our analysis shows that the model is consistent with constraints from neutrino oscillations and DM relic density as well as satisfying the current measurement on muon $g-2$. This work offers a unified framework to address neutrino masses and DM, with implications for particle physics and cosmology.

hep-ph↗

arXiv2025

Phenomenology of Inverse Seesaw Using $S_3$ Modular Symmetry

Describing neutrino masses using the inverse seesaw mechanism with discrete flavor symmetry imposed through modular forms provides a testable framework at TeV scales with fewer parameters. However, $S_3$, the smallest modular group, remains relatively underexplored. In this work, we construct the minimal supersymmetric inverse seesaw model based on the modular $S_3$ flavor symmetry. In our model, the light neutrino mass matrix depends on 6 real parameters: the complex modulus, an overall scale for light neutrino mass, a real ratio and a complex ratio of Yukawa coupling. Thanks to its minimality, our model offers various definite predictions: the lightest neutrino is massless, the neutrino masses are inverted ordering, the sum of the three light neutrino masses ($\sum_i m_i$) is 100 meV, the effective mass for the end point of the beta decay spectrum is 50 meV, the effective mass for neutrinoless double beta decay ($m_{ee}$) is in the range $38-58$ meV. In particular, the predicted values for $\sum_i m_i$ and $m_{ee}$ from our model are within reach of the next generation experiments. Our model also predicts radiative lepton flavor violating decays $\ell\to\ell'γ$ which are compatible with experimental constraints.

hep-ph↗

arXiv2024

Bounds on ALP-Mediated Dark Matter Models from Celestial Objects

We have studied the signals from axion-like particles (ALPs) as dark matter mediators from celestial objects such as neutron stars, brown dwarfs or white dwarfs. We consider the accumulation of dark matter inside the celestial objects using the multiscatter capturing process. The production of ALP from the dark matter annihilation can escape the celestial object and decay into gamma-rays and neutrinos before reaching the Earth. We investigate our model using gamma-ray observations from Fermi and H.E.S.S. and neutrino observations from IceCube and ANTARES. The effective Lagrangian approach allows us to place constraints on the ALP-photon and ALP-fermion couplings. In the gamma-ray channel, our results are able to rule out the existence of ALP with mass up to $\sim \mathcal{O}(10)$ GeV. On the other hand, the neutrino observations can be used to probe a higher mass range with ALP mass up to $\sim \mathcal{O}(100)$ GeV.

hep-ph↗

arXiv2024

Rényi Holographic Dark Energy

In this work, the holographic dark energy model is constructed by using the non-extensive nature of the Schwarzschild black hole via the Rényi entropy. Due to the non-extensivity, the black hole can be stable under the process of fixing the non-extensive parameter. A change undergoing such a process would then motivate us to define the energy density of the Rényi holographic dark energy (RHDE). As a result, the RHDE with choosing the characteristic length scale as the Hubble radius provides the late-time expansion without the issue of causality. Remarkably, the proposed dark energy model contains the non-extensive length scale parameter additional to the standard $Λ$CDM model. The cosmic evolution can be characterized by comparing the size of the Universe to this length scale. Moreover, the preferable value of the non-extensive length scale is determined by fitting the model to recent observations. The results of this work would shed light on the interplay between the thermodynamic description of the black hole with non-extensivity and the classical gravity description of the evolution of the Universe.

gr-qc↗

arXiv2024

Neutrino phenomenology in the modular $S_3$ seesaw model

We have studied neutrino phenomenology in the supersymmetric type-I seesaw model endowed with the $Γ_2 \simeq S_3$ modular symmetry. We have identified different realizations of the $S_3$ modular symmetry, referred to as models A, B, C, and D. The 4 models are compatible with neutrino mass being inverted ordering (IO). Moreover, models A, B, and D can also accommodate normal ordering (NO) neutrino masses. We identify parameter space for each model compatible with neutrino oscillation at the 2-$σ$ level. We then proceed to study the neutrino phenomenology of each model. We find that the lightest neutrino mass can be as light as 0.64 meV in the case of NO in model A and 50 meV in the case of IO in model D. The smallest effective electron neutrino mass attainable in our analysis is 8.8 meV in the case of NO (model A), and 50 meV for IO (model D). Finally, we note that the effective Majorana mass can be as small as 0.33 meV in the case of NO (model A) and 22 meV for IO (model D).

hep-ph↗

arXiv2024

Dark Photon Bremsstrahlung and Ultra-High-Energy Cosmic Ray

A dark photon is a hypothetical particle that is similar to a photon with a small mass and interacts very weakly with ordinary matter through a kinetic mixing with the ordinary photon. In this paper, we propose a new way to probe the existence of dark photons through the Bremsstrahlung effect on ultra-high-energy cosmic rays (UHECRs). Using the standard soft photon calculation, we demonstrate that the dark photon Bremsstrahlung process could lead to significant energy loss for protons in the ultralight dark photon scenario, and that this effect could be tested against observational data of UHECRs. We also provide exclusion limits which can be compared with existing limits on ultralight dark photons.

hep-ph↗

arXiv2023

Effects of odderon spin on helicity amplitudes in $pp$ elastic scattering

In recent years, the discovery of the odderon, a colorless $C$-odd gluonic compound, has been confirmed in the TOTEM and D0 collaborations. However, the spin quantum number of the odderon remains unidentified. In this work, we aim to attribute a spin of $J=3$ to the odderon in $pp$ elastic scattering by calculating the helicity amplitudes and the corresponding complex parameter $r_5$, the ratio of helicity's single-flip to non-flip amplitudes, for the spin-3 tensor odderon with the standard spin-2 tensor pomeron exchanges. Then, we apply these results to the constraints obtained from the STAR experiment at RHIC. By comparing to the contributions of the spin-1 vector odderon and spin-2 tensor pomeron, we demonstrate that the spin-3 tensor odderon, i.e. $J=3$, provides a better explanation for the observable in $pp$ elastic scattering.

hep-ph↗

arXiv2023

Odderon as Regge oddball spin-3 in $pp$ and $p\bar p$ elastic scattering

In this work, we propose that the odderon is a Regge odd-glueball tensor spin-3. To demonstrate our proposal, we study the $pp$ and $p\bar p$ elastic scattering by including contributions of the spin-3 odderon and spin-2 pomeron exchange in the processes. The phenomenological effective Lagrangian approach is used to calculate the $pp$ and $p\bar p$ elastic scattering amplitudes at the tree level. In addition, a Donnachie-Landschoff ansatz of the odderon and pomeron propagators has been used in this work. We fit the theoretical results with the various experimental data of the $pp$ and $p\bar p$ scattering at the TeV scale to determine the model parameters in the present work. By using the model parameters, the Chew-Frautschi plot of the tensor odderon Regge trajectory is evaluated. As a result, the odderon spin-3 mass is predicted to be 3.2 GeV. In addition, the total cross-section of our model is compatible with the results from TOTEM and its extrapolation from D0 collaboration. Moreover, the total cross-section also satisfies the Friossart bound at the Regge limit.

hep-ph↗

arXiv2022

Holographic Dark Energy from the Anti-de Sitter Black Hole

The anti-de Sitter (AdS) black hole plays an important role in the holographic principle. In this study, the upper bound in energy corresponding to the mass of the Schwarzschild black hole is modified to be that of the AdS black hole. Via the correspondence between the ultraviolet (UV) and infrared (IR) cutoffs, the constant term in the energy density of the holographic dark energy (HDE) can be obtained from the negative cosmological constant from the black hole. Interestingly, the proposed dark energy model could drive the late-time expansion of the Universe without the causality violation. The cosmic evolution is investigated by choosing the Hubble and particle horizons as the IR length scales. It is found that the accelerated expansion at late time can be obtained for both cases. This result may shed light on the connection between the AdS black hole and the de Sitter (dS) spacetime in the context of cosmology.

gr-qc↗

arXiv2022

Mixing Particle Production for Relaxion Mechanism

We consider the production of two heavy gauge bosons as a relaxation stopping mechanism. In this work, we analyse the conditions for a tachyonic mode for a linear combination of gauge bosons and show that the criteria are significantly different than the single gauge boson case. Moreover, the implementation of the mechanism on the $U(1)'$ model is demonstrated. We discuss various constraints for the relaxion mechanism. The phenomenology of the heavy gauge boson is also explored. We finally show a benchmark point of parameter space considering all constraints from relaxion and the $U(1)'$ mixing sector.

hep-ph↗

arXiv2021

Dark Matter and Dark Energy from a Kaluza-Klein inspired Brans-Dicke Gravity with Barotropic Fluid

We study the Kaluza-Klein inspired Brans-Dicke model with barotropic matter. Following from our previous work, the traditional Kaluza-Klein gravity action is introduced with an additional scalar field and 2 gauge fields. The compactification process results in a Brans-Dicke model with a dilaton coupled to the tower of scalar fields whereas a gauge field from 5-dimensional metric forms a set of mutually orthogonal vectors with 2 additional gauge fields. The barotropic matter is then introduced to complete a realistic set up. To demonstrate the analytical solutions of the model, we consider the case in which only 2 lowest modes becoming relevant for physics at low scale. After derivation, equations of motion and Einstein field equations form a set of autonomous system. The dynamical system is analysed to obtain various critical points. Interestingly, by only inclusion of barotropic matter, the model provides us the critical points which capable of determining the presences of dark matter, dark energy and phantom dark energy.

gr-qc↗