arXiv subjects

Yungui Gong

Publications and source records attributed to Yungui Gong.

At least 37 records · Page 2Linked to original sources

arXiv2025

Observational constraints on inflationary models with non-minimally derivative coupling by ACT

The most recent data release from the Atacama Cosmology Telescope (ACT) reveals a larger value of the scalar spectral tilt $n_s$, ruling out a broad class of inflationary attractors. In this paper, we consider inflationary models including the power law potential, the hilltop model, the polynomial $α$-attractor and exponential $α-$attractor, with non-minimally derivative coupling in the high friction limit, and show how the models can fit ACT data. We also derive constraints on the model parameters using the latest ACT data.

gr-qc↗

arXiv2025

Primordial Black Hole Formation and Spin in Matter Domination Revisited

In this article, we calculate the mass distribution of primordial black holes (PBHs) formed in the matter-dominated (MD) era by the peak theory. We apply the Zel'dovich approximation to track the nonlinear evolution of overdensities and compute the PBH abundance and mass function by incorporating a PBH formation criterion based on the hoop conjecture. We find that the PBH abundance $β$ follows the scaling law $β\simeq A_γσ_h^{*5}$ for $σ_h^*\ll 1$. Here, $σ_h^*$ is the quantity that characterizes the variance of the density fluctuation at the horizon entry. We also find that, in contrast to the previous estimates, the PBH spin is very small for $σ_h^*\ll 1$ but could be larger for larger $σ_h^*$ and broader power spectra. Finally, specializing to a monochromatic power spectrum, we prove analytically that the PBH mass distribution becomes effectively monochromatic and reveal that the resultant PBH abundance is approximately 19 times the previous prediction.

gr-qc↗

arXiv2025

Rescattering of non-minimal coupling scalar particles during inflation

We investigate the rescattering effects arising from non-minimally coupled scalar particles $χ$ that are suddenly produced during inflation. The coupling term $ξR χ^2$ significantly enhances resonant particle production compared to minimal coupling scenarios. Consequently, the produced $χ$ particles rescattering off the homogeneous inflaton condensate $ϕ$, generating abundant $δϕ$ quanta within very short time intervals. This process leads to characteristic enhancements in the power spectrum of primordial curvature perturbations at scales corresponding to the moments of particle production. When this occurs at small scales, the power spectrum amplitude can reach as high as $\mathcal{O}(10^{-2})$. Furthermore, analysis of the equilateral bispectrum shows that this mechanism also induces substantial non-Gaussian features.

astro-ph.CO↗

arXiv2025

Null tests with Gaussian Process

We investigate the null tests of spatial flatness and the flat $Λ$CDM model using the Baryon Acoustic Oscillation (BAO) data measured by the Dark Energy Spectroscopic Instrument (DESI), the cosmic chronometers (CCH) $H(z)$ data, and the Union3 and Pantheon Plus type Ia supernovae (SNe Ia) datasets. We propose a novel non-parametric reconstruction of $F_{AP}$, $D_M/r_d$ and $D'_M/r_d$ from the DESI BAO data to perform the $Ok$ diagnostic, and we also conduct the $Ok$ diagnostic using the combination of CCH and SNe Ia data. The novel method avoids the issue of the dependence on cosmological parameters such as the value of the Hubble constant. There is no evidence of deviation from the flat $Λ$CDM model, nor is there any indication of dynamical dark energy found in the observational data. Since we employ a non-parametric reconstruction method, all the conclusions drawn in this paper remain robust and agnostic to any cosmological model and gravitational theory.

astro-ph.CO↗

arXiv2025

Observational constraints on inflationary decoherence with polynomial attractor model

The quantum-to-classical transition of inflationary perturbations remains an unresolved fundamental problem, and quantum decoherence is one of the promising solutions. By considering quantum perturbations during inflation as an open quantum system interacting with its environment, quantum decoherence can be described by the Lindblad equation. This formalism modifies the evolution of primordial quantum perturbations and consequently alters the power spectrum of curvature perturbations, leading to observable consequences. In this paper, we examine the decoherence process of a polynomial attractor model featuring an ultra-slow-roll stage, extending previous analyses limited to slow-roll scenarios. We numerically compute the correction to the power spectrum due to quantum decoherence, and the results show significant modification only on large scales, with a peak generated by the decoherence correction at the minimum of the power spectrum. Using observational constraints on the scalar spectral index and the tensor-to-scalar ratio, and requiring complete decoherence for relevant scales by the end of inflation, we obtain the constraint on the interaction parameter as $10^{-17}\text{Mpc}^{-1}<k_γ<0.061\text{Mpc}^{-1}$.

gr-qc↗

arXiv2025

Detecting dilute axion stars constrained by fast radio bursts in the Solar System via stimulated decay

Fast radio bursts (FRBs) can be explained by collapsing axion stars, imposing constraints on the axion parameter space and providing valuable guidance for experimental axion searches. In the traditional post-inflationary model, axion stars could constitute up to $75\%$ of the dark matter component, suggesting that some axion stars may exist within the Solar System. Photons with energy half the axion mass can stimulate axion decay. Thus, directing a powerful radio beam at an axion star could trigger its stimulated decay, producing a detectable echo. Using this method, we find it is possible to test the existence of dilute axion stars with maximum masses ranging from $6.21\times10^{-12}M_\odot$ to $2.61\times10^{-10}M_\odot$, as constrained by FRBs, within the Solar System. The resulting echo from axion stars constrained by FRBs could be detectable by terrestrial telescopes. Detecting such an echo would confirm the existence of axion stars, unravel the mystery of dark matter, and provide key evidence that some FRBs originate from collapsing axion stars. Furthermore, FRBs produced by axion star collapses could serve as standard candles, aiding in the resolution of the Hubble tension. If no echo is detected using this method, it would place constraints on the abundance of dark matter in the form of dilute axion stars with maximum masses in the range of $6.21\times10^{-12}M_\odot$ to $2.61\times10^{-10}M_\odot$.

hep-ph↗

arXiv2025

Non-minimal coupling in light of ACT

The latest ACT data release disfavors the attractor $n_s=1-2/N$. In inflationary models with nonminimal coupling, such attractors typically arise in the strong coupling limit. To align with observational constraints, we focus on nonminimal coupling models with small coupling constants. For the model with the coupling function $Ω(ϕ) = 1 + ξf(ϕ)$ and the potential $V(ϕ) = λ^2 f^2(ϕ)$, we find that observational data constrain the parameters as $0.1 \lesssim ξ\lesssim 35$ and $0 \lesssim k \lesssim 1.5$ for $f(ϕ) = ϕ^k$ at the $1σ$ confidence level. With the help of the nonmiminal coupling $Ω(ϕ) = 1 + ξϕ^2$, the hilltop inflation and power-law inflation models with power indices $2/3$ and $1/3$ can be consistent with observational data within the $1σ$ range. We also give the viable parameter regions for $ξ$ for these three models.

astro-ph.CO↗

arXiv2025

Understanding curvature-matter interaction in viable $f(R)$ dark energy models: A dynamical analysis approach

We employ a linear stability analysis approach to explore the dynamics of matter and curvature-driven dark energy interactions within the framework of two types of viable $f(R)$ gravity models. The interaction is modeled via a source term in the continuity equations, $\mathcal{Q} = α\tildeρ_{\rm m} \Big{(}\frac{3H^3}{κ^2 ρ_{\rm curv}} + \frac{κ^2 }{3H}ρ_{\rm curv} \Big{)}$. Our results reveal significant modifications to the fixed points and their stability criteria compared to traditional $f(R)$ gravity analyses without matter-curvature coupling. We identify constraints on model and coupling parameters necessary for critical point stability, illustrating how the interaction influences cosmic dynamics within specific parameter ranges. The findings are consistent with observed cosmic evolution, supporting stable late-time acceleration. Moreover, we highlight the coupling parameter's potential role in addressing the cosmic coincidence problem.

gr-qc↗

arXiv2024

Probing the equation of state of neutron stars with captured primordial black holes

Gravitational waves (GWs) from primordial black holes (PBHs) inspiraling within neutron stars (NSs) -- should they exist -- are detectable by ground-based detectors and offer a unique insight into the internal structure of NSs. To provide accurate templates for GW searches, we solve Einstein's equations within NSs and calculate the orbital motion of the captured PBH by considering dynamical friction, accretion, and gravitational radiation. Equipped with precise GW waveforms for PBHs inspiraling inside NSs, we find that the Einstein Telescope can differentiate between various equations of state for NSs. As PBHs inspiral deeper into NSs, the GW frequency rises near the surface, then decreases to a constant value deeper within NSs. The distinctive characteristics of GW frequency serve as the smoking gun for GW signals emitted by PBHs inspiraling inside NSs and can be used to probe the nuclear matter in the crust and core of NSs.

gr-qc↗

arXiv2024

On the evidence of dynamical dark energy

To elucidate the robustness of the baryon acoustic oscillation (BAO) data measured by the Dark Energy Spectroscopic Instrument (DESI) in capturing the dynamical behavior of dark energy, we assess the model dependence of the evidence for dynamical dark energy inferred from the DESI BAO data. While the DESI BAO data slightly tightens the constraints on model parameters and increases the tension between the Chevallier-Polarski-Linder (CPL) model and the $Λ$CDM model, we find that the influence of DESI BAO data on the constraint of $w_0$ is small in the SSLCPL model. In comparison to the CPL model, the tension with the $Λ$CDM model is reduced for the SSLCPL model, suggesting that the evidence for dynamical dark energy from DESI BAO data is dependent on cosmological models. The inclusion of spatial curvature has little impact on the results in the SSLCPL model.

astro-ph.CO↗

arXiv2024

Probing new fundamental fields with Extreme Mass Ratio Inspirals

We examine extreme mass ratio inspirals (EMRIs), where a charged compact object spirals into a supermassive black hole, in modified gravity theories with additional scalar or vector fields. Using the Teukolsky and generalized Sasaki-Nakamura formalisms, we provide the post-Newtonian expansion of the energy flux of the vector waves up to $O(v^5)$ beyond the quadrupole formula in the weak field and numerically calculate the energy flux in the strong field for a charged particle moving in circular orbits. Our findings reveal a degeneracy in the scalar and vector charge parameters for weak-field, slow-motion orbits. However, for strong-field, fast-motion orbits close to the innermost stable circular orbit, we observe distinct behaviors between scalar and vector fields. We investigate the potential of using EMRIs detected by space-based gravitational-wave detectors, such as the Laser Interferometer Space Antenna to identify whether a black hole carries a scalar or vector charge. The influence of scalar and vector flux on the orbital evolution and tensor GW phase can not help us distinguish scalar and vector fields. However, extra polarizations emitted by the scalar or vector field can break the correlations between the scalar field and vector field and then help us distinguish the scalar and vector field.

gr-qc↗

arXiv2024

Extreme mass ratio inspirals in galaxies with dark matter halos

Using an analytic, static, and spherically symmetric metric for a Schwarzschild black hole immersed in a dark matter (DM) halo with the Hernquist-type profile, we derive analytic expressions for the orbital period and precession of eccentric extreme mass ratio inspirals (EMRIs) surrounded by DM halos, and we show how the precession rates decrease and even undergo a prograde-to-retrograde precession transition if the density of DM halo is large enough. The presence of local DM halos also retards the decrease of the semi-latus rectum and the eccentricity. The orbital evolution of EMRIs immersed in DM halos is then calculated numerically by considering the combined effects of gravitational radiation reaction, dynamical friction, and accretion. Comparing the number of orbital cycles accumulated over a one-year evolution for EMRIs with and without DM halos, we find that DM halos with compactness as small as $10^{-5}$ can be detected. From the mismatch between gravitational waveforms of EMRIs with and without DM halos, we show that EMRIs in galaxies can be used to probe the existence of DM halos and detect the compactness of DM halos as small as $10^{-5}$. Employing the Fisher information matrix method, we find that larger compactness and density values of DM halos help to reduce the estimation error of parameters and further break the degeneracy between the parameters.

gr-qc↗

arXiv2024

Sky localization of space-based detectors with time-delay interferometry

The accurate sky localization of gravitational wave (GW) sources is an important scientific goal for space-based GW detectors. The main differences between future space-based GW detectors, such as Laser Interferometer Space Antenna (LISA), Taiji, and TianQin, include the time-changing orientation of the detector plane, the arm length, the orbital period of the spacecraft and the noise curve. Because of the effects of gravity on three spacecraft, it is impossible to maintain the equality of the arm length, so the time-delay interferometry (TDI) method is needed to cancel out the laser frequency noise for space-based GW detectors. Extending previous work based on equal-arm Michelson interferometer, we explore the impacts of different first-generation TDI combinations and detector's constellations on the sky localization for monochromatic sources. We find that the sky localization power is almost unaffected by the inclusion of the TDI Michelson $(X, Y, Z)$ combination in the analysis. We also find that the variation in the sky localization power for different TDI combinations is entirely driven by the variation in the sensitivities of these combinations. For the six particular TDI combinations studied, the Michelson $(X, Y, Z)$ combination is the best for source localization.

gr-qc↗

arXiv2024

Distinguishing dark matter halos with Extreme mass ratio inspirals

Using the static, spherically symmetric metric for a black hole (BH) immersed in dark matter (DM) halo characterized by Hernquist, Burkert, and Navarro-Frenk-White (NFW) density distributions, we calculate the orbital periods and precessions, along with the evolution of the semi-latus rectum and eccentricity for extreme mass ratio inspirals (EMRIs) surrounded by DM halos. For the Hernquist model, we find that the gravitational force exerted by the central BH is decreased by DM halos, while DM halos put additional gravitational force on the SCO. The presence of both Burkert-type and NFW-type DM halos enhances the gravitational force acting on the SCO, resulting in a decrease in the period $P$, with the decrease depending on $M/a_0^2$; additionally, we find that the reduction in orbital precession due to DM halos is influenced by $M/a_0^2$. The presence of DM halos leads to a slower evolution of EMRIs within Hernquist-type halos, while it accelerates evolution for EMRIs in Burkert-type and NFW-type halos; furthermore, it slows the decrease of eccentricity across all three types of DM halos. By calculating the number of orbital cycles and the gravitational waveform mismatches among these three types of DM halos, as well as between scenarios with and without DM halos, we find that DM halos can be detected when $M/a_0>10^{-5}$, $M/a_0>10^{-3}$, and $M/a_0>10^{-3}$ for Hernquist-type, NFW-type, and Burkert-type DM halos, respectively. Additionally, we can distinguish between NFW-type and Burkert-type DM halos when $M/a_0> 10^{-3}$; NFW-type and Hernquist-type DM halos, as well as Burkert-type and Hernquist-type DM halos, can be distinguished when $M/a_0> 10^{-5}$.

gr-qc↗

arXiv2024

The constraint on modified black holes with extreme mass ratio inspirals

The low-energy effective action of String Theory introduces corrections to the dilaton-graviton sector, resulting in deformed black holes beyond general relativity. We analyze extreme mass-ratio inspiral systems (EMRIs), where a stellar-mass object spirals into a slowly rotating supermassive black hole including a distinct deviation parameter. This study examines the effects of this deformation on gravitational wave fluxes, orbital evolution, and phase dynamics, incorporating leading-order post-Newtonian corrections. With one-year observations of EMRIs, we employ the Fisher information matrix method to evaluate the potential for detecting deviations from general relativity through space-based gravitational wave detectors that utilize time-delay interferometry to suppress laser noise. The constraint on modified black holes, $Δα\preceq 10^{-5}$, is almost the same with and without the time-delay interferometry combination. This analysis enhances our understanding and underscores the crucial role of observations in advancing gravitational phenomena within String Theory.

gr-qc↗

arXiv2024

Nonexistence of quantum black and white hole horizons in an improved dynamic approach

In this paper, we study the quantum geometric effects near the locations where classical black hole horizons used to appear in Einstein's classical theory, within the framework of an improved dynamic approach, in which the internal region of a black hole is modeled by the Kantowski-Sachs (KS) spacetime and the two polymerization parameters are functions of the phase space variables. Our detailed analysis shows that the effects are so strong that black and white hole horizons of the effective quantum theory do not exist at all and instead are replaced by transition surfaces, across which the metric coefficients and their inverses are smooth and remain finite, as are the corresponding curvatures, including the Kretschmann scalar. These surfaces always separate trapped regions from anti-trapped regions. The number of such surfaces is infinite, so the corresponding KS spacetimes become geodesically complete, and no black and white hole-like structures exist in this scheme.

gr-qc↗

arXiv2024

Generalized approach for the perturbative dynamical braneworld in $D$ dimensions

In this paper, we propose an approach to derive the brane cosmology in the $D$-dimensional braneworld model. We generalize the "bulk-based" approach by treating the 4-brane as a small perturbation to the $D$-dimensional spherically symmetric spacetime. The linear corrections from a static 4-brane to the metric are derived from the linearized perturbation equations, while the nonlinear corrections are found by a parameterization of the perturbed metric solution. We use a time-dependent generalization to give the nonlinearly perturbed metric solution for the dynamical braneworld model, and analyse the stability of the model under the motion of the 4-brane. Through the fine tuning, we can recover the Friedmann equations for the universe with and without an effective cosmological constant. More importantly, the de Sitter expansion of the universe can be reproduced.

hep-th↗

arXiv2024

Analytical models of supermassive black holes in galaxies surrounded by dark matter halos

In this Letter, we present five analytical models in closed forms, each representing a supermassive black hole (SMBH) located at the center of a galaxy surrounded by dark matter (DM) halo. The density profile of the halo vanishes inside twice the Schwarzschild radius of the hole and satisfies the weak, strong, and dominant energy conditions. The spacetime are asymptotically flat, and the difference among the models lies in the slopes of the density profiles in the spike and regions far from the center of the galaxy. Three of them represent cusp models, whereas the other two represent core models. With the well-known (generalized) Newman-Janis algorithm, rotating SMBHs with DM halos can be easily constructed from these models.

gr-qc↗