Journal of High Energy Astrophysics最新文献_第3页

Probing cosmic isotropy with gamma-ray bursts: A dipole and quadrupole analysis of BATSE and Fermi GBM data 用伽马射线暴探测宇宙各向同性：对BATSE和费米GBM数据的偶极子和四极子分析

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2026-01-06 DOI: 10.1016/j.jheap.2026.100549

Debosi Mondal, Biswajit Pandey, Amit Mondal

The cosmological principle, asserting large-scale homogeneity and isotropy, underpins the standard model of cosmology. Testing its validity using independent astronomical probes remains crucial for understanding the global structure of the Universe. We investigate the angular distribution of Gamma-Ray Bursts (GRBs) using two of the most comprehensive all-sky datasets available, the BATSE (CGRO) and Fermi GBM catalogs, to test the isotropy of the GRB sky at large angular scales. We perform spherical harmonic decomposition of the GRB sky maps and estimate the dipole and quadrupole amplitudes. Statistical significance is evaluated by comparing the observed multipole amplitudes against distributions derived from 500 Monte Carlo realizations of isotropic skies. Our results show that the observed dipole amplitudes for both BATSE and Fermi GBM datasets lie within the 1σ region of their respective null distributions. However, the quadrupole amplitude in the raw, uncorrected BATSE and Fermi GBM skies appears elevated at 3.7σ and 3.0σ, respectively. After incorporating the BATSE sky exposure function, this apparent quadrupole anisotropy vanishes, indicating that instrumental non-uniformities fully account for the signal in that case. Owing to the absence of a publicly available full-sky exposure model for Fermi GBM, the Fermi analysis is restricted to the raw sky distribution. Our method’s reliability is validated through controlled simulations, which show it can detect the injected dipoles in BATSE-sized isotropic skies. These findings reinforce the statistical isotropy of the GRB sky and underscore the importance of accurate exposure corrections in cosmological anisotropy analyses.

宇宙学原理主张大规模的同质性和各向同性，是宇宙学标准模型的基础。使用独立的天文探测器测试其有效性对于理解宇宙的整体结构仍然至关重要。我们研究了伽玛射线暴（GRBs）的角度分布，使用了两个最全面的全天数据集，BATSE （CGRO）和Fermi GBM目录，以在大角度尺度上测试GRB天空的各向同性。我们对GRB的天空图进行了球谐分解，并估计了偶极子和四极子振幅。通过比较观测到的多极振幅与500个各向同性天空的蒙特卡罗实现的分布来评估统计显著性。我们的研究结果表明，在BATSE和Fermi GBM数据集上观测到的偶极子振幅都位于它们各自零分布的1σ区域内。然而，在原始的、未校正的BATSE和Fermi GBM天空中，四极振幅分别升高到3.7σ和3.0σ。在结合BATSE天空曝光函数后，这种明显的四极各向异性消失了，表明仪器的不均匀性完全解释了这种情况下的信号。由于缺乏公开可用的费米GBM全天曝光模型，费米分析仅限于原始天空分布。通过控制仿真验证了该方法的可靠性，结果表明该方法可以探测到batse大小的各向同性天空中注入的偶极子。这些发现加强了GRB天空的统计各向同性，并强调了在宇宙学各向异性分析中精确曝光校正的重要性。

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引用次数: 0

On the hadronic origin of the very high energy γ-ray emission surrounding the young massive stellar cluster Westerlund 1 围绕年轻大质量星团Westerlund 1的高能γ射线发射的强子起源

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2026-01-20 DOI: 10.1016/j.jheap.2026.100560

Zhaodong Shi , Rui-Zhi Yang

The Westerlund 1 (Wd 1) is the most massive known young star cluster in the Galaxy, and an extended γ-ray source HESS J1646-458 surrounding it has been detected up to 80 TeV in the very high energy, implying that cosmic rays (CRs) are accelerated effectively in the region. However, the dominant radiation process contributing to the γ-ray emission is not well constrained. In the present work, we develop a model of CR acceleration at the termination shock in the superbubble inflated by the interaction of the cluster wind from the Wd 1 with the surrounding interstellar medium. We then calculate the flux and radial profile of γ rays produced by the inelastic collisions of the hadronic CRs with the ambient gas. Our results with reasonable parameters can explain well the spectrum and radial profile of the γ-ray emission of HESS J1646-458, and consequently the γ-ray emission of HESS J1646-458 is likely to be of hadronic origin.

Westerlund 1 （Wd 1）是银河系中已知质量最大的年轻星团，其周围的扩展γ射线源HESS J1646-458在高能中被探测到高达80 TeV，这意味着宇宙射线（cr）在该区域被有效加速。然而，导致γ射线发射的主要辐射过程并没有得到很好的约束。在本工作中，我们建立了一个由Wd - 1星团风与周围星际介质相互作用而膨胀的超泡在终止激波处的CR加速模型。然后，我们计算了强子cr与周围气体的非弹性碰撞产生的γ射线的通量和径向分布。在合理的参数下，我们的结果可以很好地解释HESS J1646-458的γ射线发射光谱和径向分布，因此HESS J1646-458的γ射线发射可能是强子源的。

引用次数: 0

Probing generalized emergent dark energy with DESI DR2 用DESI DR2探测广义涌现暗能量

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2025-12-03 DOI: 10.1016/j.jheap.2025.100518

Vipin Kumar Sharma , Himanshu Chaudhary , Sanved Kolekar

As an update on the initial findings of DESI, the new results provide the first hint of potential deviations from a cosmological constant (

ω = - 1

), which, if confirmed with significance

> (2 - 4) σ

, would challenge the validity of Λ within the ΛCDM model. We explore the Generalized Emergent Dark Energy (GEDE) model using recent BAO measurements from DESI DR2, Type Ia supernova compilations, and CMB distance priors. Employing nested sampling, we constrain the parameter Δ, which characterizes deviations from ΛCDM. Our analysis shows that with CMB+DESI DR2 alone, GEDE tends to prefer positive values of Δ. However, when different SNe Ia calibrations are included, the model favors negative values of Δ, corresponding to an earlier injection of dark energy. The Marginalized constraints on ω(z) further shows that GEDE sharply emerges but then asymptotes to

ω = - 1

without crossing it. At z ∼ 1 data, GEDE provides a better fit than ΛCDM, while at z ≲ 0.5 the data favor

ω > - 1

, bringing the model deviate from ΛCDM. Bayesian model comparison shows weak support for GEDE with CMB+DESI DR2 (

\ln B F = 1.96

), moderate with PP (

\ln B F = 2.65

), weak-to-moderate with Union3 (

\ln B F = 2.34

), and weak with DES-SN5Y (

\ln B F = 1.44

). Overall, GEDE is consistent with current data and mildly favored when SNe Ia are included, making it a viable extension of ΛCDM that merits further investigation with future high precision measurements.

作为DESI初始发现的更新，新结果提供了宇宙常数（ω= - 1）的潜在偏差的第一个提示，如果以显著性>；(2−4)σ得到证实，将挑战ΛCDM模型中Λ的有效性。我们利用最近来自DESI DR2、Ia型超新星汇编和CMB距离先验的BAO测量来探索广义涌现暗能量（GEDE）模型。采用嵌套抽样，我们约束了参数Δ，它表征了与ΛCDM的偏差。我们的分析表明，单独使用CMB+DESI DR2时，GEDE倾向于选择Δ的正值。然而，当包括不同的超新星Ia校准时，模型倾向于负值Δ，对应于更早的暗能量注入。ω(z)上的边缘约束进一步表明GEDE急剧出现，但随后渐近线到ω= - 1而没有越过它。在z ~ 1数据处，GEDE提供了比ΛCDM更好的拟合，而在z ~ 0.5数据处，数据更倾向于ω>；−1，使模型偏离ΛCDM。贝叶斯模型比较显示，CMB+DESI DR2对GEDE的支持弱（lnBF=1.96）， PP对GEDE的支持中等（lnBF=2.65）， Union3对GEDE的支持弱至中等（lnBF=2.34）， DES-SN5Y对GEDE的支持弱（lnBF=1.44）。总的来说，GEDE与目前的数据一致，并且在包括超新星Ia时稍微受到青睐，使其成为ΛCDM的可行扩展，值得在未来的高精度测量中进一步研究。

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引用次数: 0

Constraining black hole shadows in dunkl spacetime using CUDA numerical computations 利用CUDA数值计算约束dunkl时空中的黑洞阴影

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2025-12-25 DOI: 10.1016/j.jheap.2025.100541

Saad Eddine Baddis, Adil Belhaj, Hajar Belmahi, Maryem Jemri

With the help of CUDA high-performance numerical codes exploited in machine learning, we investigate the shadow aspect of new rotating and charged black holes using the Dunkl derivative formalism. Precisely, we first establish the corresponding metric function encoding the involved physical properties including the optical character. Exploiting such accelerated simulations, we approach the horizon radius behaviors in order to determine the regions of the moduli space providing physical solutions. Applying the Hamilton-Jacobi mechanism, we assess the shadow aspect for non-rotating and rotating solutions. Using such an aspect, we evaluate the energy rate of emission. Developing a high-performance CUDA numerical code, we derive strict constraints on the Dunkl deformation parameters in order to establish a link with the shadow observations provided by the Event Horizon Telescope collaboration.

借助机器学习中CUDA高性能数值代码的帮助，我们使用Dunkl导数形式主义研究了新的旋转带电黑洞的阴影方面。准确地说，我们首先建立了相应的度量函数，编码所涉及的物理性质，包括光学特性。利用这种加速模拟，我们接近视界半径行为，以确定模空间的区域，提供物理解决方案。应用Hamilton-Jacobi机制，我们评估了非旋转和旋转解的阴影方面。利用这一角度，我们计算了发射的能量率。我们开发了一个高性能的CUDA数值代码，推导了对Dunkl变形参数的严格约束，以便与事件视界望远镜合作提供的阴影观测建立联系。

引用次数: 0

Multifrequency evolution of the integrated pulse profile of radio pulsars by implementing the inverse compton mechanism 利用逆康普顿机制实现射电脉冲星综合脉冲谱的多频演化

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2026-01-12 DOI: 10.1016/j.jheap.2026.100557

Tridib Roy , Mayuresh Surnis , Mageshwaran Tamilan , Monalisa Halder , Siddhartha Biswas

The Main Aim of this paper is to explain the emergence of new components of pulsars at higher radio bands by implementing the Inverse Compton Scattering Mechanism. From pulsar radio observation, it is seen that a couple of pulsars reveal new emission components at higher radio frequencies, although they show single-component emission at lower frequencies. We develop a brief outline, fostering inverse Compton scattering (ICS) of the low-frequency radio photons as a vulnerable source of scattering, susceptible to explaining the evolution of new components of some radio pulsars at higher bands. We couple the conventional curvature radiation (CR) mechanism and ICS, and suggest that the spectral convolution of the flux component individually from CR and the modulated template due to the ICS scattered component can be combined to reproduce such signatures associated with the diverse morphology of the integrated pulse profile. We reproduce the beam frequency diagram, the geometrical variation of different parameters of the emission geometry, as well as the multi-frequency evolution from theory. We have suitably tuned the input parameter space and given the combination of parameters that can tune to a particular scattered frequency in tabulated form. We conclude that ICS may be a responsible process for describing the emergence of new components in higher radio emission bands.

本文的主要目的是利用逆康普顿散射机制来解释高波段脉冲星新成分的出现。从脉冲星射电观测中，可以看到一对脉冲星在较高的无线电频率上显示出新的发射成分，尽管它们在较低的频率上显示出单一成分的发射。我们发展了一个简短的大纲，培养低频无线电光子的逆康普顿散射（ICS）作为一个脆弱的散射源，容易解释一些射电脉冲星在更高波段的新成分的演变。我们将传统的曲率辐射（CR）机制与ICS进行了耦合，并提出可以将来自CR的通量分量的光谱卷积和由ICS散射分量引起的调制模板相结合，以再现与集成脉冲剖面的不同形态相关的这些特征。我们从理论上再现了波束频率图、发射几何形状不同参数的几何变化以及多频演化。我们已经适当地调整了输入参数空间，并给出了可以以表格形式调整到特定散射频率的参数组合。我们得出的结论是，ICS可能是描述更高无线电发射波段新成分出现的负责任的过程。

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引用次数: 0

Decoding Cygnus X-2: The critical role of reflection in IXPE data 解码Cygnus X-2: IXPE数据中反射的关键作用

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2026-01-12 DOI: 10.1016/j.jheap.2026.100548

Honghui Liu , Jiachen Jiang , Adam Ingram , Cosimo Bambi , Andrew C. Fabian , Ruben Farinelli , Renee Ludlam , Nathalie Degenaar , Jakub Podgorny , Andrea Santangelo , James F. Steiner , Andrew J. Young , Zuobin Zhang

We present a spectro-polarimetric re-analysis of the first IXPE observation of Cygnus X-2 which we determine to be mainly in the normal branch, from quasi-simultaneous observations with NuSTAR, NICER, and INTEGRAL. We measure the hard X-ray polarization angle and find it to be consistent with the previously measured position angle of the radio jet. Leveraging NuSTAR’s detection of both the relativistic Fe K emission line and the Compton hump, we constrain the flux contribution of the reflected emission from the inner accretion disk to be 10% of the total X-ray flux in the IXPE energy band. Unlike previous studies that modeled only the Fe K emission line, we fit the full-band reflection spectrum using a fully relativistic disk model. A polarization degree of approximately 20% for the reflection component could explain the hard X-ray polarization data from IXPE. We also discuss the inferred disk inclination angle derived from our spectro-polarimetric modeling.

我们提出了对天鹅座X-2的第一次IXPE观测的光谱偏振重新分析，我们确定主要是在正常分支，从与NuSTAR， NICER和INTEGRAL的准同时观测。我们测量了硬x射线偏振角，发现它与先前测量的射电喷流位置角一致。利用NuSTAR对相对论性Fe - K发射线和康普顿驼峰的探测，我们将内吸积盘反射发射的通量贡献限制为IXPE能带中x射线总通量的10%。不像以前的研究只模拟了Fe - K发射线，我们使用了一个完全相对论的圆盘模型来拟合全波段反射光谱。反射分量的偏振度约为20%，可以解释IXPE的硬x射线偏振数据。我们还讨论了从我们的光谱偏振模型推导出的圆盘倾角。

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引用次数: 0

Search for γ-ray emission from dwarf spheroidal galaxies with Fermi-LAT data 用Fermi-LAT数据搜索矮球状星系的γ射线发射

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2025-12-29 DOI: 10.1016/j.jheap.2025.100536

Shang Li

This study uses approximately 17 years of Fermi-LAT data to search for γ-ray emission from 45 Milky Way dwarf spheroidal galaxies (dSphs, including candidates). No significant ( > 5σ) γ-ray signal is found in the scenarios of dark matter annihilations. Very weak γ-ray excesses ( >  2 σ) are found in some dSphs. The most significant signal for dark matter annihilation is observed toward Willman 1, the peak TS value is  ∼  9.6 at a dark matter mass  ∼  60 GeV for the annihilation channel

χ χ \to τ^{+} τ^{-}

. Due to the low significance of the signal, its true origin cannot be determined at the moment. The observed γ-ray excess in the vicinity of Reticulum II shows variation, indicating that the signal is unlikely to be attributable to dark matter annihilation. Furthermore, the γ-ray excesses in Eridanus II and Reticulum III are significantly offset from their centers, possibly due to contamination from astrophysical sources. Three other targets (Boötes II, Ursa Minor and Crater II) show local significance between 2 - 2.5σ, whereas the corresponding cross-sections are inconsistent with the stringent limits from the stacked analysis of dSphs, ruling out a dark matter annihilation origin.

这项研究使用了大约17年的Fermi-LAT数据来搜索45个银河系矮球状星系（dSphs，包括候选星系）的γ射线发射。在暗物质湮灭的情况下，没有发现显著的（ >； 5σ） γ射线信号。在一些dSphs中发现了非常弱的γ射线过量（ >； 2 σ）。在Willman 1方向观测到暗物质湮灭的最显著信号，在暗物质质量 ~ 60 GeV处，湮灭通道的TS峰值为 ~ 9.6,χχ→τ+τ−。由于该信号的显著性较低，目前无法确定其真正的来源。在II网附近观测到的γ射线过量显示出变化，表明该信号不太可能归因于暗物质湮灭。此外，Eridanus II和Reticulum III的γ射线过量可能由于天体物理源的污染而与它们的中心发生了显著的偏移。另外三个目标（Boötes II，小熊星座和陨石坑II）在2 - 2.5σ之间具有局部意义，而相应的横截面与dSphs叠加分析的严格限制不一致，排除了暗物质湮灭起源。

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引用次数: 0

Exploring the spectral characteristics of the periodic burster 4U 1323-62: Type-I X-ray burst and persistent emission 探索周期爆发4U 1323-62的光谱特征：i型x射线爆发和持续发射

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2025-12-31 DOI: 10.1016/j.jheap.2025.100545

Mahasweta Bhattacharya , Aditya S. Mondal , Biplab Raychaudhuri , Gulab C. Dewangan

We report on the results obtained by the analysis of persistent and type-I thermonuclear X-ray burst emission observed from the periodic burster 4U 1323-62. These analyses are based on the NuSTAR observation performed on 2024 August 7, for a total exposure of around 90 ks. The persistent emission is well described by an absorbed thermal Comptonization model. An absorption edge is also detected at an energy of  ∼  7.42 keV, which indicates the presence of absorbing material in the vicinity of this system. Six bursts have been observed during this observation, wherein we find the burst recurrence time to be 4.52 ± 0.32 hr. All the bursts exhibit the characteristics of a sharp rise and exponential decay. We perform the time-resolved spectroscopy of the burst spectra described by a model consisting of thermal emission from the neutron star surface and a varying persistent emission component to study the evolution of burst parameters. The enhancement of the persistent emission during burst exposure is characterized by the scaling parameter f_a, which reflects the increasing strength of the burst-disc interaction with burst intensity, likely driven by Poynting-Robertson drag. The spectral analysis of bursts estimate the average apparent blackbody emitting radius of the neutron star to lie within 1.5-3.5 km. The ignition depths computed from the burst parameters indicate short Type-I thermonuclear bursts from a mixed hydrogen-helium fuel layer.

我们报告了通过分析从周期爆发4U 1323-62观测到的持续和i型热核x射线爆发发射获得的结果。这些分析是基于2024年8月7日进行的核星观测，总曝光量约为90公里。用吸收热复合模型很好地描述了持续辐射。在能量为 ~ 7.42 keV处也检测到吸收边，这表明在该系统附近存在吸收物质。在这次观测中观察到6次爆发，其中我们发现爆发的重复时间为4.52 ± 0.32小时。所有的爆发都表现出急剧上升和指数衰减的特征。我们对由中子星表面的热发射和变化的持续发射成分组成的模型所描述的爆发光谱进行了时间分辨光谱分析，以研究爆发参数的演变。在爆发暴露期间持续发射的增强表现为尺度参数fa，这反映了爆发盘相互作用的强度随着爆发强度的增加而增加，可能是由Poynting-Robertson阻力驱动的。对爆发的光谱分析估计，中子星的平均表观黑体发射半径在1.5-3.5 公里之间。根据爆炸参数计算的点火深度表明，混合氢氦燃料层发生了短时间的i型热核爆炸。

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引用次数: 0

Hamilton-Jacobi analysis of noncanonical inflation in f(R, T) gravity: Constraints from planck/ACT data, and theoretical bounds f（R， T）引力中非正则暴胀的Hamilton-Jacobi分析：来自普朗克/ACT数据的约束和理论边界

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2025-12-11 DOI: 10.1016/j.jheap.2025.100531

Zohdieh Ossoulian, Tayeb Golanbari, Khaled Saaidi

The latest CMB data from ACT DR6, in combination with Planck, DESI, and BICEP/Keck, indicate a slight upward shift in the scalar spectral index. This trend puts several previously favored inflationary models under tension. In this work, we study an inflationary scenario in the framework of f(R, T) gravity, where R is the Ricci scalar and T is the trace of the energy-momentum tensor, with a nonminimal coupling between matter and curvature. The inflaton is assumed to be a noncanonical scalar field with a generalized kinetic energy. To analyze the dynamics of inflation, we employ the Hamilton-Jacobi formalism, where the Hubble parameter is expressed as a function of the scalar field rather than the potential. Within this setup, we examine two functional forms of the Hubble parameter, a power-law and an exponential form, and derive key observables such as the scalar spectral index n_s and the tensor-to-scalar ratio r. Comparing the results with ACT DR6, we explore the parameter space of the model. We find that the power-law case fits the data well across a wide range of free parameters, while the exponential case requires a large number of e-folds to be consistent with observations. After inflation, we study reheating, where the dynamics of reheating and inflation are closely linked. Taking into account the overproduction of primordial gravitational waves constrained by the observational bound on ΔN_eff, we obtain a lower limit on the reheating temperature, which is especially restrictive for the stiff equation of state ω_re. This bound implies that the number of e-folds of inflation should generally not exceed N ≲ 64(65). The resulting energy spectrum of gravitational waves exhibits an enhanced amplitude, thereby bringing it within the observable range of upcoming detectors. We also check the consistency of the model with the Swampland conjectures and the Trans-Planckian Censorship Conjecture (TCC). Our results demonstrate that combining f(R, T) gravity with noncanonical field dynamics provides a rich and testable framework for the early universe. In addition, the Hamilton-Jacobi approach, by avoiding extra approximations, yields a clearer picture of inflation in modified gravity and opens new directions for addressing fundamental problems in high-energy cosmology.

来自ACT DR6的最新CMB数据，结合普朗克、DESI和BICEP/Keck，表明标量光谱指数略有上升。这一趋势使几个先前受欢迎的通货膨胀模型面临压力。在这项工作中，我们研究了f（R， T）引力框架下的暴胀情景，其中R是里奇标量，T是能量动量张量的迹，具有物质和曲率之间的非极小耦合。膨胀子被假定为具有广义动能的非正则标量场。为了分析暴胀的动力学，我们采用了Hamilton-Jacobi形式，其中哈勃参数被表示为标量场的函数，而不是势。在此设置中，我们检查了哈勃参数的两种函数形式，幂律形式和指数形式，并推导出关键观测值，如标量谱指数ns和张量与标量比r。将结果与ACT DR6进行比较，我们探索了模型的参数空间。我们发现幂律情况可以很好地在广泛的自由参数范围内拟合数据，而指数情况需要大量的e-fold才能与观测结果一致。在通货膨胀之后，我们研究再加热，其中再加热和通货膨胀的动态是密切相关的。考虑到原始引力波的过量产生受到ΔNeff观测界的约束，我们得到了再加热温度的下限，该下限对刚性状态方程ωre具有特别的限制。这个界意味着暴胀的e-fold的数目一般不应超过N > 64（65）。由此产生的引力波能谱显示出增强的振幅，从而使其进入即将到来的探测器的可观测范围。我们还检查了模型与沼泽猜想和跨普朗克审查猜想（TCC）的一致性。我们的研究结果表明，将f（R， T）引力与非正则场动力学相结合，为早期宇宙提供了一个丰富且可测试的框架。此外，通过避免额外的近似，Hamilton-Jacobi方法可以更清晰地描绘出修正引力下的暴胀，并为解决高能宇宙学中的基本问题开辟了新的方向。

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引用次数: 0

Late-time cosmic dynamics in f(R, Lm) gravity with recent observations f（R, Lm）引力的后期宇宙动力学与最近的观测

IF 10.5 4区物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS

Journal of High Energy Astrophysics

Pub Date : 2026-03-01 Epub Date: 2026-01-13 DOI: 10.1016/j.jheap.2026.100558

Amit Samaddar, S.Surendra Singh

In this work, we investigate the late-time cosmic dynamics in the framework of non-linear f(R, L_m) gravity, adopting the functional form

f (R, L_{m}) = \frac{R}{2} + L_{m}^{2}

. To explore the dark energy behavior, we assume an oscillatory parametric equation of state,

ω (z) = ω_{0} + b \sin [\log (1 + z)]

, which allows smooth deviations from the cosmological constant. Using a joint MCMC analysis with the latest Hubble 31 chronometer data, DESI DR2 BAO measurements, and Type Ia supernova samples (Pantheon+, DES-SN5Y and Union 3), we obtain well-constrained parameters around

H_{0} ≃ 67.6 - 67.8 km s^{- 1} {Mpc}^{- 1}

and

ω_{0} \approx - 0.47

to

- 0.48

, consistent with Planck 2018 and other current observations. The model exhibits a dynamically accelerating expansion driven by an oscillatory equation of state, satisfies the null and dominant energy conditions while violating the strong energy condition and yields present-day value

q_{0} ≃ - 0.47

to

- 0.48

, reproducing ΛCDM behavior at late times. The derived Universe ages (t₀ ≈ 13.3 Gyr) agree well with CMB and stellar constraints, confirming that the proposed oscillatory f(R, L_m) model provides an observationally consistent and dynamically viable alternative to ΛCDM cosmology.

本文采用函数形式f(R,Lm)=R2+Lm2，研究了非线性f（R,Lm）引力框架下的晚时宇宙动力学。为了探索暗能量的行为，我们假设一个振荡参数状态方程，ω(z)=ω0+bsin[log(1+z)]，它允许从宇宙常数平滑偏离。利用最新的哈勃31天文台数据、DESI DR2 BAO测量数据和Ia型超新星样本（Pantheon+、DES-SN5Y和Union 3）进行联合MCMC分析，我们得到了在H0≈67.6−67.8km−1Mpc−1和ω0≈−0.47 ~−0.48附近的良好约束参数，与普朗克2018和其他现有观测结果一致。该模型在振荡状态方程的驱动下呈现出动态加速膨胀，满足零能和优势能条件，同时违背强能条件，并产生当前值q0≃- 0.47 ~ - 0.48，再现了后期ΛCDM行为。推导出的宇宙年龄（t0 ≈ 13.3 Gyr）与CMB和恒星的约束条件很好地吻合，证实了所提出的振荡f（R, Lm）模型为ΛCDM宇宙学提供了观测上一致和动态上可行的替代方案。

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引用次数: 0