arXiv subjects

Javlon Rayimbaev

Publications and source records attributed to Javlon Rayimbaev.

At least 19 recordsLinked to original sources

arXiv2026

Axion-angle dependence of the rotational and tidal properties of PNJL quark stars

We investigate how a fixed, spatially uniform axion angle modifies the rotational and static tidal properties of self-bound quark stars in general relativity, using an axion-extended Polyakov-loop Nambu--Jona-Lasinio equation of state. We vary $θ$ from $0$ to $π$ while holding the remaining model parameters fixed, and compute the leading-order moment of inertia and the second-order spin-induced quadrupole moment and mass shift. The calculation includes finite-surface-density contributions to the rotational mass shift and static tidal response. Across this range, the static maximum mass increases from $1.68$ to $1.95\,M_\odot$, remaining below the lower edge of the quoted $1σ$ timing interval for PSR~J0740+6620. At $M=1.338\,M_\odot$, the moment of inertia increases by $13\%$ and the dimensionless tidal deformability rises from $342$ to $547$. Over the common mass range examined, the differences in the moment of inertia between adjacent sampled angles exceed the tested interpolation and table-resolution sensitivities. Despite these changes, joint fits to the five sequences describe the $\bar I$--$C$ and I-Love-Q relations with maximum departures of $2.7\%$ and $0.4\%$, respectively, over the fitted domains. The predicted binary tidal-deformability curves lie within the estimated 90\% credible region of the adopted GW170817 posterior over the mass-ratio ranges examined. Within this EOS family, stellar properties vary appreciably with $θ$, while the normalized quantities admit accurate joint fits across the five sequences.

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arXiv2026

Testing charged Simpson-Visser-AdS spacetimes with twin-peak QPOs

In this manuscript, we study circular geodesics and twin-peak high-frequency quasi-periodic oscillations (HF-QPOs) in the charged Simpson--Visser--anti-de Sitter (AdS) spacetime, which depends on a charge parameter $Q$, a regularization scale $b$ and an AdS radius $l$. Written in terms of the areal radius $R=\sqrt{r^{2}+b^{2}}$, the specific energy, angular momentum, Keplerian frequency and innermost stable circular orbit (ISCO) of test particles coincide with those of the Reissner--Nordström--AdS black hole, so $b$ enters the epicyclic spectrum only through a factor $1-b^{2}/R^{2}$ in the radial frequency. We give this frequency and the ISCO condition in closed form. We then fit the relativistic-precession model to the HF-QPO pairs of GRO~J1655$-$40 and XTE~J1550$-$564, with their dynamical masses included as Gaussian priors. The Schwarzschild limit gives $χ^{2}=32.9$ for two degrees of freedom. One additional deformation removes this tension: $Q/M=0.814^{+0.059}_{-0.074}$ at fixed $l=100M$, or $l=40.6^{+6.2}_{-4.8}\,M$ at $Q=0$, both with $χ^{2}\simeq0.13$. These two solutions lie on a single degeneracy valley in the $(Q,l)$ plane, and, at $l=100M$, $b$ is left unconstrained up to $b\simeq3.9M$ (68\%), a limit set by the charge prior rather than by the data. A Kerr black hole with spin $a\simeq0.3$--$0.4$ reproduces the same pairs, so the inferred deformation most likely absorbs the spin neglected by the static metric. Our results therefore describe degeneracies among orbital-frequency deformations; they are not a measurement of an electric charge or of a cosmological constant.

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arXiv2026

Conservative Orbital Resonance Networks as Local Environmental Diagnostics for Extreme Mass Ratio Inspirals

LLow order orbital resonances provide localized probes of the conservative geometry sampled by extreme mass ratio inspirals. We study fixed eccentricity and inclination slices of the ordered $3{:}2$, $5{:}3$, and $2{:}1$ polar to radial resonance surfaces in source consistent anisotropic black hole environments, treating rotation strictly to first order. A horizon regularized Dehnen sequence produces unequal resonance displacements, reaching $-7.17\%$, $-5.45\%$, and $-3.94\%$ in a fixed global benchmark. After matching both the total environmental mass and the enclosed mass at $10M_\bullet$, we compare Dehnen and Einasto inspired families. Two dimensionless network spacing ratios are organized primarily by the local logarithmic enclosed mass slope: for the common $β=2$ regularization their maximum cross family departure from a shared linear relation is $4.1\times10^{-4}$, while varying the horizon taper through $β=2$--$4$ increases the departure to at most $2.1\times10^{-3}$. The unequal ordering of the three resonance displacements holds at every point of a directly evaluated finite eccentricity and inclination grid. A six observable conservative response analysis is numerically full rank but strongly ill conditioned and nearly aligned with orbital nuisance directions. The result therefore establishes local conservative profile sensitivity, not unique tomography or a detector level parameter recovery forecast.

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arXiv2026

Quasibound states of charged Dirac fields around Einstein-Euler-Heisenberg black holes

We study quasibound states of a massive charged Dirac field on the Einstein--Euler--Heisenberg (EEH) black hole, the extension of Reissner--Nordström (RN) by the leading weak-field vacuum-polarization term of QED. We derive the background to first order in the Euler--Heisenberg coupling $a$. We show that it admits a nondegenerate horizon at $Q=M$ and an extremal charge $Q_{\rm ext}=M[1+a/(40M^2)+\mathcal{O}(a^2)]>M$, with horizon data that depend on $\sqrt a$ near extremality. From the separated radial equations, we derive an identity that excludes real-frequency quasibound states on any background of this class, so damped branches cannot become unstable. Since the EEH corrections first enter at $\mathcal{O}(r^{-5})$ in the electrostatic potential, the trapping condition $Mμ^2-qQω_R>0$ and the hydrogenic spectrum coincide with RN, and no fine-structure-order splitting arises. Two-sided shooting with a Muller root finder shows that the real frequencies shift only by near-zone amounts that are linear in $a$ and strongly suppressed with angular momentum. The damping rates respond in a branch-dependent way. At $Q/M=0.99$ the $\ell=0$ ground state becomes slightly longer-lived, while the $(n_r,j,\ell,λ)=(0,\tfrac32,1,-2)$ state decays up to $80\%$ faster for $a/M^2\le1$, and near the trapping threshold the damping rate increases by up to $60\%$. Switching on the metric and potential corrections separately, together with a WKB analysis of the inner barrier, identifies the mechanisms: Coulomb screening always increases leakage, while the metric correction controls the sign and size of the $\ell$-dependent effect. Characteristic time-domain evolutions with Richardson-extrapolated matrix-pencil extraction reproduce the frequency-domain shifts.

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arXiv2026

Boundary-induced corrections to the response of an Unruh-DeWitt detector outside a compact star with Robin surface conditions

We formulate the finite-time response problem for a radially accelerated Unruh--DeWitt detector coupled to a real massless scalar field outside a static, spherically symmetric, horizonless compact star. The stellar exterior is described by the Schwarzschild geometry, while unresolved field--surface interactions are represented by a local Robin condition at the stellar radius. After reducing the Klein--Gordon equation to a half-line Schrödinger problem, we identify a sufficiently stable branch of the Robin family from positivity of the radial operator, construct delta-normalized continuum modes, and define the static ground state with respect to Schwarzschild time. We derive a mode-amplitude representation of the smoothly switched detector response that avoids a direct numerical treatment of the coincidence singularity of the Wightman distribution. We obtain a radially aligned trajectory of constant signed proper acceleration in terms of the rapidity measured by static observers. The resulting formulation separates the effects of compactness, surface condition, closest approach, detector gap, and interaction duration. We also state the flat-space, Dirichlet, static-detector, low-frequency, large-distance, and long-interaction limits required to validate a numerical implementation. The framework provides a controlled extension of detector studies with static reflective compact objects to finite-time moving probes.

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arXiv2026

Magnetically charged spinning particles around a regular black hole: constraints on the monopole charge from quasi-periodic oscillations

We investigate the dynamics of magnetically charged spinning test particles in the spacetime of the Bardeen regular black hole, sourced by nonlinear electrodynamics and featuring a magnetic monopole charge parameter g. Using the Mathisson-Papapetrou-Dixon equations with the Tulczyjew spin condition, extended by the Coulomb-like force between the particle's magnetic charge and the monopole, we derive the effective potential for equatorial motion and analyze circular orbits, the innermost stable circular orbit (ISCO), superluminality constraints and high-energy collisions. Solving the ISCO conditions perturbatively around Schwarzschild, we obtain exact coefficients, r_{\rm ISCO}, and show that the magnetic coupling λg shifts r_{\rm ISCO} only at higher order while it changes the ISCO energy and angular momentum at first order. We compute radiative efficiencies (up to \simeq 8\% in the explored range, against 5.72\% for Schwarzschild) and the orbital and radial epicyclic frequencies, including the ISCO and the 3:2 resonance, whose frequency at fixed mass is shifted by 5--11\% for g/M=0.5--0.7.

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arXiv2026

Rotating black holes surrounded by PFDM in STVG: Shadows and eikonal quasinormal modes

We investigate the optical and dynamical properties of a rotating black hole in scalar--tensor--vector gravity (STVG) surrounded by perfect fluid dark matter (PFDM). Starting from the static STVG--PFDM geometry, we consider a Kerr-like rotating extension characterized by the spin parameter $a$, the STVG coupling $α$, and the PFDM parameter $λ$. We first examine the horizon structure and a radial effective mass function, then analyze null geodesics and unstable spherical photon orbits. We use these results to construct the black-hole shadow and study its size, distortion, and dependence on model parameters and observer inclination. We then compare the predicted angular shadow diameter with the Event Horizon Telescope observations of M87$^*$ and Sgr~A$^*$ in the $(a,α)$ parameter space for representative values of the PFDM parameter. The comparison shows that the PFDM contribution can shift the parameter-space region compatible with the observed shadow diameter, while the shadow size is generally less sensitive to spin than to deformation. We further estimate the Hawking energy-emission spectrum in the high-frequency geometric-optics approximation, using the shadow radius as an effective absorption scale. Finally, we study the quasinormal-mode spectrum in the eikonal limit through the correspondence between unstable photon orbits and ringdown frequencies. The numerical results recover the expected Schwarzschild limit and show a clear separation between the prograde and retrograde modes as the spin increases. The combined analysis provides a consistent optical, energy emission, and ringdown characterization of the rotating STVG--PFDM geometry.

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arXiv2026

Charged Simpson-Visser-AdS spacetime: QPOs and observational constraints

In this article, we examine particle dynamics and Quasi-periodic oscillations within a charged Simpson-Visser-Anti-de Sitter (AdS) spacetime. We first analyze the behavior of the metric and black hole horizons under the competing impact of electric charge $Q$, regularization parameter $b$, and AdS radius $l$. The roots of the metric function reveal transitions between three distinct topological classes: non-extremal configurations featuring distinct inner and outer horizons, extremal limits with a single degenerate horizon, and strictly positive, horizonless wormhole geometries. By evaluating the effective potential, we determine how this modified geometry shifts the Innermost Stable Circular Orbit (ISCO) and alters the angular momentum and energy of test particles. Moreover, we derive the Keplerian, radial, and vertical frequencies to model quasi-periodic oscillations (QPOs). We show that the interplay between the regularization parameter $b$ and the AdS radius $l$ significantly modifies twin-peak QPOs. In particular, $b$ drives fundamental QPO frequencies higher than those predicted by standard general relativistic backgrounds. Twin-peak high-frequency QPO data from two black-hole binaries disfavor the Schwarzschild limit at $\sim\!4σ$, but constrain only a degenerate combination of charge and AdS curvature, leaving the regularization parameter entirely unconstrained by the data.

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arXiv2026

Ringdown and greybody signatures of rational regular black holes in non-polynomial gravity

We study the quasinormal mode spectrum and wave-scattering properties of the four-dimensional rational regular black hole recently obtained in non-polynomial (quasi-topological) gravity. Using third-order WKB together with two independent cross-checks a Frobenius--Riccati shooting method and a time-domain evolution we compute the fundamental scalar, electromagnetic, and axial gravitational-type quasinormal frequencies, validating our approach against known Schwarzschild results. We find that as the geometry approaches extremality, its dimensionless ringing frequency is systematically suppressed relative to the Schwarzschild value, a direct and quantifiable imprint of the non-polynomial regularization that we trace, via the photon-sphere correspondence, to the response of the effective potential near the horizon. A Fisher-matrix estimate indicates that this suppression could in principle be resolved by a space-based detector such as LISA for a sufficiently massive and nearby source. We further compute, for the first time, the axial gravitational-type ringdown spectrum of this geometry using the Regge--Wheeler master equation, while noting that a full stability analysis of the underlying gravity theory remains an open problem requiring the linearized field equations of the modified action. Finally, we examine the greybody transmission factors across spins $s=0,1,2$ and show that they follow the same systematic ordering and near-extremal enhancement as the ringing-frequency suppression, pointing to a common physical origin. Together, these results give one of the first quantitative characterizations of the observational signatures and the remaining open theoretical questions of a regular black hole in modified gravity.

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arXiv2026

Pulsar magnetospheres in dynamical Chern-Simons gravity: deathline conditions and polar-cap particle acceleration

The role of surface gravity in neutron stars (NSs) is considerable in the radiation mechanisms of the surrounding plasma magnetosphere near the star surface, as they are highly magnetized, compact gravitating objects with compactness $M/R \simeq 0.2$. In this context, they serve as a celestial laboratory for testing gravity theories that dominate the stars' exteriors through plasma magnetospheric radiation. In this paper, we examine how dynamical Chern-Simons (dCS) gravity modifies pulsar electrodynamics in the slow-rotation, weak-coupling regime; the leading-order correction affects only the off-diagonal metric component $g_{tϕ}$, while the diagonal components remain as in General Relativity (GR). We first solve the Maxwell equations in the dCS framework for the electromagnetic field components and obtain analytical solutions for the electric and magnetic fields. We show that the magnetic field components are the same as in GR, while the electric field components are modified in dCS. We then derive analytic expressions for the induced electric charge density, known as the Goldreich-Julian (GJ) charge density, which sources the induced electric field arising from the magnetic field and the star's rotation. In dCS, it is larger than in the GR case, whereas the accelerating electric field parallel to the magnetic field lines is weaker. Next, we consider the deathline condition for switching off electron and positron radiation via inverse Compton scattering in the star's polar cap zone and show that the line shifts upward in the $P-\dot{P}$ diagram, explaining the physics of shorter-lived pulsars. Lastly, we study charged-particle acceleration in the polar cap region and show that electrons reach higher energies over shorter distances than in the GR case.

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arXiv2026

Probing black holes surrounded by Dust field in Quantum Fluctuation Modified Gravity with twin-peak QPOs

We study a static, spherically symmetric black hole solution surrounded by a dust field within quantum fluctuation modified gravity, in which the quantum-fluctuation parameter $α$ and the dust-field strength parameter $K$. The horizon structure reveals the two parameters acting in opposite directions: strengthening $K$ draws the inner and outer horizons together until they merge into a single extremal horizon, while a larger $α$ restores the Schwarzschild limit; the same opposing trend extends to the effective potential and the characteristic circular-orbit radii -- the innermost stable circular orbit, the marginally bound orbit, and the marginal circular orbit -- which shift inward with $K$ and outward with $α$, and to the Keplerian and radial epicyclic frequencies of massive test particles. From these frequencies we build three twin-peak quasi-periodic oscillation models -- relativistic precession, warped-disk, and epicyclic-resonance -- along with their $3{:}2$, $4{:}3$, and $5{:}4$ resonance radii, all following the same $K$-$α$ trend. Testing all three models against twin-peak QPO data from two stellar-mass (GRO~J1655$-$40, XTE~J1550$-$564) and two intermediate-mass (M82~X$-$1, NGC~1313~X$-$1) sources through a Markov Chain Monte Carlo analysis places best-fit constraints, at the $2σ$ level, of $K\in(0,0.5)$ and $α\in(0.3,0.6)$ across all sources and models.

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arXiv2026

Charged particles and QPO constraints in tidal charge black hole magnetosphere sourced by a current loop

We investigate the dynamics of charged particles in the dipolar electromagnetic field generated by a stationary current loop around a static black hole in the Randall--Sundrum braneworld model. The current loop is located at the innermost stable circular orbit (ISCO) of the tidal charged black hole, and the azimuthal electromagnetic four-potential is obtained as an exact analytical solution of the Maxwell equations in the curved background. Starting from the Hamilton--Jacobi equation, we derive the effective potential for charged particle motion in both the interior and exterior regions of the current loop, and analyze the dependence of the ISCO radius, angular momentum, energy, and orbital frequency on the tidal charge parameter $b$ and the magnetic coupling parameter $ω$. We further compute three fundamental frequencies and show that the dipolar loop field revives a nonzero nodal precession frequency even though the background is static and non-rotating. Using these frequencies we construct five twin-peak QPO models (RP, WD, and ER2--ER4) and perform a Markov chain Monte Carlo (MCMC) analysis to constrain the braneworld parameters $(b,ω)$ from the observed twin-peak QPO frequencies of six black hole sources spanning three mass regimes: GRO~J1655--40, XTE~J1550--564, GRS~1915$+$105, H~1743$+$322, M82~X-1, and Sgr~A$^{*}$. Adopting the epicyclic-resonance ER4 model as the representative framework, we find moderate, non-negligible tidal charges $b\simeq0.3$--$1.0$, while the magnetic coupling remains consistent with zero, $|ω|\lesssim0.05$. Our results therefore place upper bounds on the tidal charge and on the magnetic coupling strength from astrophysical QPO data.

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arXiv2026

Energy-momentum-squared gravity: charged quark star solutions with unified interacting matter

We investigate the equilibrium structure of electrically charged quark stars within the framework of energy-momentum-squared gravity (EMSG), adopting a unified interacting quark-matter equation of state that incorporates perturbative QCD corrections, color superconductivity, and finite-strange-quark-mass effects. By solving the modified Tolman-Oppenheimer-Volkoff equations over a broad range of EMSG coupling strengths and interaction parameters, we show that the inclusion of electric charge substantially increases both the maximum mass and radius compared with neutral configurations. For strong negative couplings and pronounced interaction strengths, the resulting stellar models reach masses close to $3,M_{\odot}$ with compactness ratios of order $0.34$, placing them within the mass range inferred for the secondary component of GW190814, whose nature remains observationally undetermined. The presence of charge reduces the central density at maximum mass by approximately $10$--$15\%$ while maintaining full compliance with causality requirements. Furthermore, comparisons with observational constraints from PSR J1614$-$2230, J0348$+$0432, J0740$+$6620, J0952$-$0607, and recent NICER radius measurements indicate that charged EMSG configurations remain consistent with current astrophysical bounds over a wide parameter space. These results demonstrate that a moderate electric charge, when combined with nonlinear matter-geometry coupling, can support quark stars that are significantly more massive than those predicted in general relativity, underscoring the potential observational relevance of charged compact objects in modified gravity and multimessenger astrophysics.

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arXiv2026

Second-order slow rotation of wormholes in Einstein-scalar-Gauss-Bonnet gravity

We investigate slowly rotating traversable wormholes in Einstein--scalar--Gauss--Bonnet gravity beyond the linear rotation regime. The static backgrounds are obtained without expanding in the Gauss--Bonnet coupling, while rotational effects are treated perturbatively up to second order. Both monopolar and quadrupolar deformations are included, allowing us to determine the spin-induced changes in the asymptotic charges, throat geometry, energy-condition behavior, and mass quadrupole. The quadrupolar equations develop an internal regular singular point, which is handled by selecting the regular local solution through a Frobenius analysis. The rotation-induced response of the throat source is incorporated consistently through the junction conditions. Independent shooting and collocation calculations of the quadrupolar sector give mutually consistent solutions. The rotating throat remains oblate throughout the fixed-coupling family, while at $χ=0.15$ the smooth-bulk near-throat radial null-energy-condition violation persists but its radial extent becomes latitude dependent. These results provide a self-consistent second-order description of rotating Einstein--scalar--Gauss--Bonnet wormholes.

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arXiv2026

Kerr-referenced analytical parametrization of rotating black holes in dynamical Chern-Simons gravity

Rotating black holes in dynamical Chern-Simons gravity are known nonperturbatively mainly through numerical solutions, which limits their direct use in strong-field applications. We construct a Kerr-referenced analytical parametrization of the near-general-relativistic numerical branch using a compact radial coordinate, low-order angular multipoles, and continued fractions. The resulting two-parameter family accurately reproduces the numerical metric throughout the validated weak-coupling and moderate-spin domain. Independent off-grid solutions confirm that the parametrization retains its accuracy away from the calibration set. We further assess the model through equatorial light rings, critical impact parameters, and full two-dimensional null-geodesic ray tracing without assuming separability. The resulting shadow observables closely match those obtained from the numerical geometries. This parametrization therefore provides a practical analytical metric for geodesic and strong-field calculations without relying on a slow-rotation expansion.

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arXiv2026

Corrected thermodynamics and radiation predictions of modified black bounce compact objects

We study the thermodynamic properties and radiation characteristics of a regular compact object obtained by applying the Simpson-Visser (SV) regularisation to the Schwarzschild modified gravity black hole. The resulting SV-MOG spacetime, whose lapse function involves both the MOG coupling parameter alpha and the black-bounce parameter l, smoothly interpolates between a regular black hole, a one-way wormhole, and a traversable wormhole depending on the parameter l. We derive the Hawking temperature and heat capacity for the black hole branch, identifying second-order phase transitions signaled by sign changes in CV, and, for the horizonless wormhole branch where no causal horizon and hence no genuine Hawking radiation exists we instead construct a physically well-defined effective temperature from the Lyapunov exponent of the unstable photon sphere. Quantum gravitational corrections to the entropy are incorporated via logarithmic terms parameterized by coefficients beta1, beta2, whose theoretically preferred ranges in loop quantum gravity and string theory we discuss, and we show that deviations from the Bekenstein-Hawking area law become significant at small horizon radii. A linear scalar-perturbation analysis further shows that the effective radial potential remains non-negative throughout the black-hole exterior and across the wormhole throat, indicating stability against monopole perturbations independently of the thermodynamic stability inferred from the heat capacity.

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arXiv2026

Weakly nonlinear strong-field signatures of spontaneously vectorized Einstein-vector-Gauss-Bonnet black holes near the Schwarzschild bifurcation

We study the static, spherically symmetric electric branch of spontaneously vectorized Einstein-vector-Gauss-Bonnet black holes close to its Schwarzschild bifurcation. A weakly nonlinear expansion is built around the fundamental vector zero mode. The critical coupling is determined independently by shooting and collocation, the second-order metric correction is checked against the unreduced covariant equations, and the corresponding ADM-mass correction is shown to vanish analytically. The leading departure of the vectorized branch from the bifurcation point follows from a third-order Fredholm solvability condition. Using the resulting metric, we calculate the leading corrections to the photon sphere, shadow scale, marginally bound orbit, innermost stable circular orbit, orbital and epicyclic frequencies, the geometric three-to-two frequency-ratio radius, the instability of the circular photon orbit, and the logarithmic strong-deflection coefficient. Near the bifurcation, the photon sphere and innermost stable orbit move outward, whereas the three-to-two radius moves inward. The photon-orbit angular frequency decreases and its Lyapunov exponent increases. These results characterize the local strong-field geometry of the electric vectorized branch. They are not intended as observational constraints or as an extrapolation to the strongly nonlinear regime.

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arXiv2026

Blandford-Znajek Scaling in a Power-Law Rotating Kalb-Ramond Geometry: Magnetic-Flux Systematics and Bayesian Identifiability

Relativistic jets from spinning black holes offer a possible strong-field probe of gravity through the Blandford-Znajek mechanism. We study the leading jet-power scaling in the four-dimensional power-law rotating Kalb-Ramond geometry introduced by Kumar, Ghosh, and Wang. The metric is used here as a stationary background, without assuming that it constitutes a newly established exact rotating solution. We first examine the deformation at the metric level. For $s=2$ it is absorbed completely by a mass redefinition, whereas for $s>2$ the correction decays more slowly than the usual mass term. Our main benchmark is therefore the nondegenerate $s=3/2$ case, whose correction falls faster than the Kerr mass term; $s=3$ is kept as a secondary comparison. We evaluate the BZ scaling under three magnetic assumptions: fixed total horizon flux, fixed local normal field with the proper horizon area, and a reduced radius-based flux proxy. The resulting trends differ appreciably, showing that the magnetic prescription is itself a leading systematic. For GRO J1655-40 and GRS 1915+105, the marginalized deformation posterior remains close to the horizon-conditioned effective prior for both a uniform prior and a truncated-Gaussian alternative. The jet-only profile likelihood is also nearly flat over the allowed deformation range, with the same qualitative behavior in the $s=3$ test. Thus, within the present setup, the jet-power proxies do not independently determine the Kalb-Ramond deformation. A stronger inference will require better control of the rotating background, source-dependent magnetic flux, non-Kerr spin estimates, and a larger sample.

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