高能暂现源 · 每日文献综述

HIGH-ENERGY TRANSIENTS · DAILY LITERATURE REVIEW
2026 年 7 月 8 日 星期三 · 数据截至 arXiv / ADS 最新收录日

本页经 8 次补录 · · · · · · · ·

I.

今日头条

No Breaking · 无突发
今日无通过复核的重大进展

当日 9 篇核心与相关文献均为常规推进,核心 3 篇已按优先级列于下方。

II.

核心文献

3 篇
0108-20 补录
优先级 85 · 伽马暴 GRB · GRB 宇宙学 · 高能暂现天体

Self-organized Criticality across Precursor, Main, and Extended Emission Phases of Gamma-Ray Bursts

伽马射线暴前兆、主发射与延展发射阶段的自组织临界性

Xiu-Juan Li, Chang-Zhi Niu, Zi-Hang Li et al.

原文摘要Abstract

We investigate the self-organized criticality (SOC) signatures of the precursor, main emission, extended emission (EE), and whole emission phases for three-phase gamma-ray bursts (GRBs). These parameters include the conventional duration-based index T<SUB>100</SUB>, as well as the newly introduced parameters T<SUB>MVT</SUB> and spectral lags (τ<SUB>32</SUB>, τ<SUB>42</SUB>). All cumulative distributions show power-law scaling in each phase for both Type I and Type II GRBs. For the first time, we demonstrate that the EE phase exhibits the same SOC scaling as the other phases. Phase-to-phase ratios show that spectral lag ratios are correlated, while duration-based ratios are not, indicating a common origin for spectral lags. Statistical comparisons among the four indexes reveal no significant differences across phases or within each phase, except in the EE phase where T<SUB>MVT</SUB> is marginally different from the spectral lags. When compared with the three-dimensional expectation α = 2.0 (duration-based), T<SUB>MVT</SUB> and T<SUB>100</SUB> show no significant deviation, whereas spectral lags seem to follow the fluence scaling α ≍ 1.5 as predicted by the fractal-diffusive SOC model. Thus, the same magnetic reconnection driven avalanche likely operates throughout the entire GRB, and these new parameters provide new observational diagnostics of the avalanche process.

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AI 综述 AI-generated · 以原文为准
亮点

首次证明延展发射(EE)阶段具有与其他阶段相同的 SOC 标度;新引入 T_MVT 与谱延迟参数为雪崩过程提供新的观测诊断。

脉络与展望

以往对 GRB 自组织临界性的研究多集中在主发射或延展发射的持续时间分布,较少系统比较前兆、主发射、延展发射和全程的统一标度行为。该文将传统 T100 与新提出的 T_MVT 及谱延迟等参数纳入同一框架,在 Type I/II GRB 各时相中均得到幂律累积分布,首次把 SOC 证据延伸到延展发射阶段。谱延迟比的相关性以及谱延迟更接近 fluence 标度 α≈1.5,提示其与持续时标参数可能追踪雪崩过程的不同侧面。从趋势看,未来可把这类多参数、多时相 SOC 诊断拓展到更大样本和更高时间分辨率,以检验磁重联雪崩图像在 GRB 全过程中的普适性。

接收 2026-07-08 · 刊出 2026-07-30 · 收录 2026-08-20

0207-22 补录
优先级 78 · X射线双星与吸积致密天体 · 高能暂现天体

Transient and Variable Ultra-luminous X-ray Sources in NGC 4552

NGC 4552中的暂现与变化超亮X射线源

V. Jithesh (Centre of Excellence in Astronomy and Astrophysics, Christ University), A. S. Sreya (Centre of Excellence in Astronomy and Astrophysics, Christ University), Riya Elza Mathew (Centre of Excellence in Astronomy and Astrophysics, Christ University), et al.

原文摘要Abstract

We searched for transient and variable X-ray sources in the elliptical galaxy NGC 4552 using the Chandra and XMM-Newton observations from 2001-2012. We detected 14 transient and variable X-ray sources within the 4R<SUB>e</SUB> region of the galaxy, which exhibited peak state and undetected flux behaviour in the Chandra observations. Among them, two sources (T1 and T14) exceed the X-ray luminosity <inline-formula><tex-math id="TM0001" notation="LaTeX">$10^{39}\rm ~erg~s^{-1}$</tex-math></inline-formula> in the detected observations and have the peak state and undetected luminosity ratio of ≥14.3 and ≥8.7, respectively, which we classified as transient and variable ultra-luminous X-ray sources (ULXs). For the third relatively bright transient source, the flux varies by a factor of 3 across the detected observations, and the hardness ratio analysis suggests a normal X-ray binary system. The remaining sources have luminosities in the <inline-formula><tex-math id="TM0002" notation="LaTeX">$10^{37}-10^{38} \rm ~erg~s^{-1}$</tex-math></inline-formula> range, and the spectral analysis indicates that the sources may belong to neutron star or black hole X-ray binary systems, either in the hard or thermal-dominated state. The identified transient and variable ULXs exhibited high variability and soft spectral characteristics, which are consistent with ULXs accreting at super-Eddington rates. The near-infrared (NIR) counterpart search using JWST observations identified potential NIR counterparts for three mildly variable sources, and their magnitudes in different NIR bands suggest a red supergiant companion for each source. Deep X-ray monitoring observations can shed further light on the new transient and variable ULXs.

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AI 综述 AI-generated · 以原文为准
亮点

首次在NGC 4552中系统识别暂现ULX,发现两个峰值光度>10^39 erg/s的源(T1和T14),并结合JWST近红外数据找到三个可能的红超巨星对应体。

脉络与展望

对邻近星系中暂现X射线源的系统搜索已揭示多种源类型,包括X射线双星和ULX(Williams+ 2008; Jithesh+ 2016)。本研究在椭圆星系NGC 4552中通过分析十多年的Chandra与XMM-Newton观测,识别出14个暂现与变化源,其中T1和T14的峰值光度超过10^39 erg/s,增添了新的暂现ULX成员。近期工作表明暂现ULX可能代表超爱丁顿吸积的过渡阶段(Robba+ 2022; Allak 2023),而本工作发现的源展现出软谱与高变异性,与超临界吸积特征相符。未来深度X射线监测和光学/红外对应体研究将有助于阐明这些源的吸积物理与演化。

预印本 2026-07-08 · 刊出 2026-07-09 · 收录 2026-07-22

0308-24 补录
优先级 75 · 太阳耀斑 · 日冕物质抛射 · MHD模拟

Data-based Magnetohydrodynamic Simulation of a Flare Eruption in Active Region 13663 Associated with a Tilted Coronal Mass Ejection

基于数据的磁流体动力学模拟活动区13663耀斑爆发伴随倾斜日冕物质抛射

Nian Liu, Satoshi Inoue, Ju Jing et al.

原文摘要Abstract

We conducted data-constrained magnetohydrodynamic (MHD) simulations of the X1.3 flare produced in solar active region 13663 on 2024 May 5, at 11:41 UT. The simulations employed the zero-beta MHD approximation, with initial conditions derived from the nonlinear force-free field (NLFFF) extrapolated from Helioseismic and Magnetic Imager vector magnetograms. Anomalous resistivity was applied in the NLFFF to locally enhance magnetic reconnection and create more highly twisted field lines that lead to the eruption. We successfully reproduced the dramatic eruption in the simulations with anomalous resistivity, and found good agreement with Atmospheric Imaging Assembly extreme-ultraviolet observations. The simulation shows that the initially sheared magnetic field lines can evolve into an erupting magnetic flux rope (MFR) through tether-cutting reconnection occurring near either of their footpoints. Furthermore, the direction of the erupting MFR is significantly influenced by the location of enhanced reconnection. This arises from changes in the MFR's magnetic connectivity, which in turn modify the Lorentz forces acting upon it. This study highlights that subtle details in the flare-triggering process can shape the subsequent evolution of a coronal mass ejection (CME), offering valuable insights for future CME modeling and space weather prediction.

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AI 综述 AI-generated · 以原文为准
亮点

在NLFFF中施加反常电阻以局部增强磁重联,成功再现爆发,并指出耀斑触发中的细微差异可改变磁绳磁连接和洛伦兹力,进而塑造CME方向,为空间天气预报提供新思路。

脉络与展望

该工作延续了利用非线性无力场外推和零β磁流体动力学模拟研究太阳活动区爆发的主流思路,但进一步通过局部反常电阻控制重联位置,系统考察爆发磁绳的方向变化。结果显示,磁绳的磁连接变化会改变其所受洛伦兹力,从而影响日冕物质抛射的传播方向。这表明耀斑触发过程中的精细结构对CME演化具有重要作用。未来可结合更完整的热力学过程、多波段观测约束以及集合模拟,以提高CME方向与到达时间的预测能力,服务空间天气预报。

接收 2026-07-08 · 刊出 2026-08-17 · 收录 2026-08-24

边缘相关 7 篇 · 低相关性展开 +
优先级 20 · 多信使触发与联合 · 由暂现源样本驱动的总体统计、宇宙学与基础物理应用07-22 补录

Scaling Relations for Binary Black Hole Merger Times from Cosmological Initial Conditions

François, Thibaut L., Gualandris, Alessia, Dehnen, Walter

原文摘要Abstract

Recent evidence from Pulsar Timing Arrays (PTAs) for a nanohertz gravitational wave background is broadly consistent with theoretical expectations from a population of massive black hole binaries (MBHBs), although the inferred amplitude appears somewhat higher than predicted by standard models. Interpreting these observations requires a robust understanding of the merger timescales of MBHBs, and of their connection to host galaxy properties. In this work, we investigate the evolution of MBHBs selected from cosmological galaxy mergers in the ILLUSTRISTNG simulation. We re-simulate these systems at high resolution using the N-body code GRIFFIN to accurately resolve the dynamical friction and stellar hardening phases, and follow their evolution to coalescence with a semi-analytical model. We find that cosmological galaxy encounters and the resulting MBHBs are typically highly eccentric. We characterise the distribution of binary eccentricities at formation and at entry into the PTA band, and quantify the corresponding residence times. We identify the key parameters governing the duration of the different stages of MBHB evolution, and derive scaling relations linking galaxy and orbital properties to dynamical friction, hardening, and total coalescence times. These relations provide a framework for subgrid prescriptions in cosmological simulations. Applying these scaling relations to the full ILLUSTRISTNG merger population, we infer the probability distributions of galaxy merger and black hole coalescence times. We find that galaxy mergers typically complete within ~0.7 Gyr, while the total black hole coalescence time is ~1.0 Gyr. These short timescales imply efficient binary evolution, consistent with current PTA constraints.

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宇宙学初始条件下双黑洞并合时标的标度关系 · 基于ILLUSTRIS-TNG模拟和GRIFFIN再模拟,研究了双黑洞从形成到并合的演化,推导了并合时标与星系和轨道性质的标度关系,并应用于整个模拟样本,发现典型并合时标约为0.7-1.0 Gyr。

预印本 2026-07-08 · 刊出 2026-07-09 · 收录 2026-07-22

优先级 10 · 太阳日冕 · 可见光连续谱 · 太阳物理

Structure and Dynamics of the Inner Corona Measured from the DEB Initiative 2024 Eclipse Image Sequence

Matthew J Penn, Robert Baer, Chris Mandrell, et al.

原文摘要Abstract

The Dynamic Eclipse Broadcast (DEB) Initiative citizen science program observed coronal visible continuum brightness during the 2024 April 8 total eclipse from locations across North America. We present results from 11 DEB sites spanning 2700 km of distance and showing 49 minutes of evolution. The coronal brightness radial profiles from these telescopes are tightly correlated from 1.2 to 4.0 solar radii and comparable to published photometric coronal intensities. The coronal flattening parameter is measured from 1.4 to 2.8 solar radii. A Ludendorff index of 0.0761 +/- 0.0007 is computed but the extrapolation techniques used by some to calculate this index are shown to disagree with this direct measurement, and alternate structure parameters are suggested. Measured radial velocities are compared with an MHD model of the corona during the eclipse from Y. Li et al. (2026). A polar downflow is measured with an average radial velocity of -37 +/- 3 km s-1 and a deceleration of 14 +/- 3 m s-2 at a speed and position which agrees with the model. The predicted mixture of outflows and downflows at low heights is seen, as well as outflows in two western regions of the corona. The fastest observed outflow has a radial speed of 105 km s-1 and is likely associated with a transient event not predicted by the model. Future DEB Initiative eclipse experiments can more tightly constrain models of the inner corona by using both coronal intensity and radial velocity measurements.

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从DEB倡议2024日食图像序列测量的内冕结构与动力学 · 利用DEB倡议2024年日食期间11个站点的观测,分析了内冕的亮度径向分布、扁平化参数和Ludendorff指数,并测量了极向下降流与局部外流的速度,与MHD模型对比验证了预测并发现未预测的瞬态事件。

预印本 2026-07-14 · 接收 2026-07-08 · 刊出 2026-07-20 · 收录 2026-07-18

优先级 10 · 高能暂现天体 · 黑洞08-20 补录

Analytically Approximate Black Hole Solution to Higher Curvature Gravity

Seyed Naseh Sajadi

原文摘要Abstract

Higher-curvature gravity usually leads to very complicated field equations, which makes it hard to find analytical solutions. In this work, we obtain analytical charged black hole solutions in higher-curvature gravity by using black hole thermodynamics and the continued fraction expansion. We study the thermodynamics of static black holes using the first law of thermodynamics and the Smarr formula. We show that our results agree with those obtained by directly solving the field equations in Einstein gravity.

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高曲率引力的解析近似黑洞解 · 通过黑洞热力学和连分数展开,在高曲率引力中获得解析带电黑洞解,并验证其与爱因斯坦引力直接求解结果一致。

预印本 2026-08-03 · 刊出 2026-07-08 · 收录 2026-08-20

优先级 1008-24 补录

Prospects of indirect detection of dark matter via primordial black hole induced gravitational waves

Paul, Debarun, Haque, Md Riajul, Pal, Supratik

原文摘要Abstract

Primordial black holes (PBHs), produced in the early Universe, can source a stochastic background of induced gravitational waves (GWs) and provide a non-thermal origin for dark matter (DM). We investigate DM production in a PBH-dominated cosmological framework, including contributions from PBH evaporation, gravitational production, and thermal freeze-in and freeze-out mechanisms, and determine the regions consistent with the observed DM relic abundance. We find that thermal freeze-in can compensate for the underabundance of PBH-sourced DM, while indirect detection remains largely insensitive due to the feeble interaction strength, making future GW observatories such as LISA and the Einstein Telescope (ET) unique probes of this scenario. For freeze-out DM, indirect detection experiments constrain regions with relatively large annihilation cross-sections, whereas GW observations probe complementary regions with heavier DM masses and smaller interaction strengths. Consequently, the same DM parameter space cannot be simultaneously probed by both indirect detection searches and GW missions. These results establish GW observations as a powerful and independent probe of DM production in PBH-dominated cosmologies, opening a new observational window into DM properties and the thermal history of the pre-BBN Universe.

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原初黑洞诱导引力波间接探测暗物质的前景 · 研究原初黑洞主导宇宙中暗物质的多种产生机制,并论证引力波观测可作为间接探测的独立互补探针。

接收 2026-07-08 · 刊出 2026-08-17 · 收录 2026-08-24

优先级 1008-31 补录

Observational Limits on Einasto Dark Matter Parameters from Event Horizon Telescope Images of Sgr A<SUP>∗</SUP> and M87<SUP>∗</SUP>

Errehymy, A., Hansraj, S., Hansraj, C.

原文摘要Abstract

The Event Horizon Telescope (EHT) has provided images of the supermassive black holes Sgr A* and M87*, enabling direct tests of gravity. Any extended mass distribution, such as a dark matter halo, perturbs null geodesics in the photon-ring regime, making shadow measurements a probe of inner-halo structure. In this work, we investigate static, spherically symmetric black holes surrounded by Einasto-type dark matter halos and derive constraints from EHT shadow data. Starting from the Einasto density profile with parameters <inline-formula> <mml:math><mml:msub><mml:mrow><mml:mi>ϱ</mml:mi></mml:mrow><mml:mrow><mml:mn>0</mml:mn></mml:mrow></mml:msub><mml:mo>,</mml:mo><mml:mover><mml:mrow><mml:mi>α</mml:mi></mml:mrow><mml:mrow><mml:mo>∼</mml:mo></mml:mrow></mml:mover><mml:mo>,</mml:mo><mml:mover><mml:mrow><mml:mi>ν</mml:mi></mml:mrow><mml:mrow><mml:mo>∼</mml:mo></mml:mrow></mml:mover></mml:math> </inline-formula>, we construct a metric function <inline-formula> <mml:math><mml:mi>f</mml:mi><mml:mo>(</mml:mo><mml:mi>r</mml:mi><mml:mo>)</mml:mo><mml:mo>=</mml:mo><mml:mn>1</mml:mn><mml:mo>-</mml:mo><mml:mn>2</mml:mn><mml:mi>M</mml:mi><mml:mo>/</mml:mo><mml:mi>r</mml:mi><mml:mo>+</mml:mo><mml:mn>2</mml:mn><mml:msub><mml:mrow><mml:mi>M</mml:mi></mml:mrow><mml:mrow><mml:mi>∞</mml:mi></mml:mrow></mml:msub><mml:mover><mml:mrow><mml:mi>g</mml:mi></mml:mrow><mml:mrow><mml:mo>∼</mml:mo></mml:mrow></mml:mover><mml:mo>(</mml:mo><mml:mi>r</mml:mi><mml:mo>)</mml:mo></mml:math> </inline-formula> that interpolates between the black hole horizon and the asymptotic halo, following the approach of Xu et al. but adapted specifically to the Einasto scenario. We analyze the photon potential, null geodesics, and shadow radius as functions of black hole mass M in the nonspinning limit. Using the dimensionless shadow diameter d<SUB>sh</SUB> ≡ Dθ/M measured by the EHT---<inline-formula> <mml:math><mml:msubsup><mml:mi>d</mml:mi><mml:mrow><mml:mspace></mml:mspace><mml:mtext>sh</mml:mtext><mml:mspace></mml:mspace></mml:mrow><mml:mrow><mml:mi>M</mml:mi><mml:mn>87</mml:mn><mml:mo>*</mml:mo></mml:mrow></mml:msubsup><mml:mo>=</mml:mo><mml:mn>11.0</mml:mn><mml:mo>±</mml:mo><mml:mn>1.5</mml:mn></mml:math> </inline-formula> and <inline-formula> <mml:math><mml:msubsup><mml:mi>d</mml:mi><mml:mrow><mml:mspace></mml:mspace><mml:mtext>sh</mml:mtext><mml:mspace></mml:mspace></mml:mrow><mml:mrow><mml:mi>Sgr</mml:mi><mml:mspace></mml:mspace><mml:mi>A</mml:mi><mml:mo>*</mml:mo></mml:mrow></mml:msubsup><mml:mo>=</mml:mo><mml:mn>9.5</mml:mn><mml:mo>±</mml:mo><mml:mn>1.4</mml:mn></mml:math> </inline-formula>---we perform Bayesian parameter estimation to identify allowed regions in the Einasto parameter space. Combined with the independently measured black hole masses from stellar dynamics, our results place constraints on the inner dark matter distribution: for Sgr A*, adopting the stellar-orbit mass prior, we find ϱ<SUB>0</SUB> ≲ 10<SUP>-11</SUP> M<SUB>⊙</SUB> pc<SUP>-3</SUP> at 1σ confidence, while for M87*, the bounds are weaker due to distance uncertainties. The Einasto index <inline-formula> <mml:math><mml:mover><mml:mrow><mml:mi>ν</mml:mi></mml:mrow><mml:mrow><mml:mo>∼</mml:mo></mml:mrow></mml:mover></mml:math> </inline-formula> is weakly constrained, indicating that EHT precision primarily limits the mass enclosed near the photon sphere rather than the profile slope. These findings demonstrate that horizon-scale imaging can complement galactic-scale dynamics in probing dark matter models, including fuzzy dark matter scenarios with solitonic cores. Future EHT observations will refine these constraints and distinguish between competing dark matter descriptions.

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基于事件视界望远镜对Sgr A*和M87*图像的Einasto暗物质参数观测限制 · 利用EHT阴影数据约束Einasto暗物质晕参数,发现主要限制光子球附近质量而非轮廓斜率。

接收 2026-07-08 · 刊出 2026-08-26 · 收录 2026-08-31

优先级 10 · 太阳耀斑、硬X射线爆发、地球伽马闪 TGF09-09 补录

An Approximate Bayesian Deep Learning Approach for Uncertainty-aware Differential Emission Measure Estimates in the Solar Corona from the SDO

N. Balodhi, R. J. Morton

原文摘要Abstract

Accurately estimating the temperature distribution of solar coronal plasma, known as the Differential Emission Measure (DEM), is vital for understanding the thermodynamics of the corona and associated heating. However, recovering the DEM from multispectral observations like those from the Atmospheric Imaging Assembly (AIA) on board NASA's Solar Dynamics Observatory (SDO) is a mathematically ill-posed, underdetermined problem, and traditional regularization-based inversion methods are computationally intensive and provide limited uncertainty quantification. We present a deep learning framework for DEM reconstruction that incorporates Monte Carlo Dropout to perform approximate Bayesian inference, yielding per-pixel empirical distributions over the DEM that characterize epistemic or systematic model uncertainty in the learned inversion. The network is trained with a dual-head architecture supervising both AIA image reconstruction and DEM fidelity, with non-negativity enforced by construction. The network is trained directly on real SDO/AIA observations along with the associated DEM solutions from regularized inversion. We validate performance against both synthetic thermal distributions and real coronal data, demonstrating accurate recovery of thermal structure across a range of plasma conditions, while maintaining significant computational efficiency over traditional inversion techniques. This method ensures physically legitimate, non-negative solutions and provides per-pixel uncertainties, making it a reliable, high-speed, and uncertainty-aware tool for large-scale solar data analysis.

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一种基于近似贝叶斯深度学习的SDO太阳日冕微分发射度估计不确定性方法 · 提出用蒙特卡洛Dropout的深度学习框架从SDO/AIA图像重建DEM,提供逐像素不确定性且高效。

预印本 2026-09-07 · 接收 2026-07-08 · 刊出 2026-08-10 · 收录 2026-09-09

优先级 507-27 补录

Local Geometric Bounds on Generalized Entropy Evolution along Null Horizons

Erik Bertram

原文摘要Abstract

We develop a local and covariant framework for constraining the evolution of generalized entropy along null horizons, combining classical geometric methods with constraints from quantum field theory. Building on the quantum focusing conjecture (QFC), which restricts entropy evolution along null directions, we derive a Raychaudhuri-type differential inequality for the generalized expansion that makes its local dependence on expansion and shear explicit. The resulting relation, $\frac{dΘ}{dλ} \le -θΘ+ \tfrac{1}{2}θ^2 - σ^2$, reveals a direct interplay between expansion and shear in controlling entropy flow: shear contributes negatively and yields a monotonic suppression of the generalized expansion in shear-dominated regimes, while expansion provides a competing geometric source term. This structure provides a local geometric formulation consistent with the QFC and clarifies its interpretation as a constraint on entropy evolution. We further show that quantum extremal surfaces correspond to configurations characterized by $Θ=0$, whose local stability properties are governed by the same geometric data. In addition, we derive a bound on the exponential separation of nearby null generators, indicating that the same combination of expansion and shear also controls geometric instability. Our results provide a local geometric refinement of entropy bounds in semiclassical gravity and establish a direct connection between null geometry, quantum energy conditions, and entropy flow, offering a local geometric perspective on horizon thermodynamics beyond global formulations.

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沿零视界的广义熵演化的局部几何界限 · 本文结合经典几何与量子场论约束,发展了一个局部协变框架,推导出广义膨胀的雷乔杜里型微分不等式,揭示了剪切和膨胀在控制熵演化中的直接相互作用,并证明了量子极端面对应的几何配置与稳定性条件。

预印本 2026-07-23 · 刊出 2026-07-08 · 收录 2026-07-27