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Images in axially symmetric gravitational lenses from elliptical sources: the elimination method 椭圆源轴对称引力透镜中的图像:消除法
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-11-19 DOI: 10.1007/s10509-024-04378-4
Albert Kotvytskiy, Štefan Parimucha

This work focuses on developing an analytical method for constructing images in gravitational lenses. Building on our previously proposed elimination method, which utilized algebraic geometry for constructing images from circular sources, this study emphasizes images from elliptical sources using axially symmetric gravitational lenses. We detail the rational parameterization of an arbitrarily located source and use our algorithm to derive an expression that determines all images for an arbitrary axially symmetric gravitational lens. To validate this expression, we considered several limiting cases leading to well-known results. Specifically, we examined two simple models: a single-point lens and a homogeneous disk lens. By placing an elliptical source at the origin of the source plane and reducing it to a circle, we reproduced all previously known images, such as the Einstein ring for a single-point lens, and a double Einstein ring for a disk lens. Additionally, we demonstrated the Construction of images in other arbitrary lens-source configurations.

这项工作的重点是开发一种在引力透镜中构建图像的分析方法。我们之前提出的消除方法利用代数几何构建了来自圆形源的图像,在此基础上,本研究强调利用轴对称引力透镜构建来自椭圆源的图像。我们详细介绍了任意位置源的合理参数化,并使用我们的算法推导出一个表达式,该表达式可确定任意轴对称引力透镜的所有图像。为了验证这个表达式,我们考虑了导致众所周知的结果的几种限制情况。具体来说,我们研究了两个简单的模型:单点透镜和同质圆盘透镜。通过在光源平面的原点放置一个椭圆光源并将其缩小为一个圆,我们重现了所有之前已知的图像,如单点透镜的爱因斯坦环和圆盘透镜的双爱因斯坦环。此外,我们还展示了其他任意透镜-光源配置下的图像构造。
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引用次数: 0
Following the tidal trail: a history of modeling the Magellanic Stream 追寻潮汐踪迹:麦哲伦海流建模史
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-11-18 DOI: 10.1007/s10509-024-04377-5
Scott Lucchini

The formation of the Magellanic Stream has puzzled astronomers for decades. In this review, we outline the history of our understanding of the Magellanic System highlighting key observations that have revolutionized thinking of its evolution. We also walk through the major models and theoretical advances that have led to our current paradigm − (1) the LMC and SMC have just had their first pericentric passage around the Milky Way, having approached recently as a bound pair; (2) the LMC and SMC have had several tidal interactions in which material has been stripped out into the Trailing Stream and Leading Arm; (3) the LMC hosted an ionized gas circumgalactic medium which envelops the Clouds and the neutral Stream today, providing the bulk of the associated mass; and (4) the Milky Way’s circumgalactic gas provides strong ram pressure and hydrodynamic forces to shape the morphology of the Magellanic System including the formation of a bow shock due to the LMC’s supersonic approach.

麦哲伦星系的形成几十年来一直困扰着天文学家。在这篇综述中,我们将概述我们对麦哲伦星系的认识历史,重点介绍那些彻底改变了麦哲伦星系演化思想的关键观测数据。(1) LMC 和 SMC 刚刚经历了第一次绕银河系的同心圆运动,它们最近才作为一对结合体靠近银河系;(2) LMC 和 SMC 经历了几次潮汐相互作用,物质被剥离到尾流和前臂中;(4) 银河系的环星系气体提供了强大的冲压力和流体动力,塑造了麦哲伦系统的形态,包括由于 LMC 的超音速接近而形成的弓形冲击。
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引用次数: 0
Investigation of non-substorm Pi2 magnetic pulsation during solar flare event 太阳耀斑事件期间非次级风暴 Pi2 磁脉冲研究
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-11-18 DOI: 10.1007/s10509-024-04375-7
Islam Hawash, Essam Ghamry, Susan W. Samwel, Muhamed Yousef Omar, Hala El-Desoky

Pi2 magnetic pulsations have been observed to occur at low latitudes when the magnetosphere is in a near ground state and substorm activity would be expected to have ceased. In the present study, we report a global non-substorm Pi2 magnetic micro-pulsations occurred, for the first time, during a solar flare event. We investigate this Pi2 at two different locations: in the inner magnetosphere using Van Allen Probe A (VAP-A) satellite, and ground-based magnetic stations located in Japan-Korea, Africa, and America sectors. By comparing the horizontal component of ground stations with the electric and magnetic components within the magnetosphere, we report a global Pi2 starting nearby at 12:05 UT lasting to 12:11 UT during the ejection of a solar flare with X9.3-class that have had its peak flux at 12:02 UT on 6 September 2017. We study the Pi2 oscillations at Kakioka (KAK) station and VAP-A satellite through wavelet analysis. By analyzing the high-latitude stations, we find that the Pi2 event has a good correlation with a Poleward Boundary Intensification (PBI).

据观测,当磁层处于接近地面状态,亚暴活动预计已经停止时,Pi2 磁脉冲会在低纬度地区发生。在本研究中,我们首次报告了在太阳耀斑事件期间发生的全球非亚暴 Pi2 磁微脉冲。我们在两个不同地点对 Pi2 进行了研究:利用 Van Allen Probe A(VAP-A)卫星在内磁层,以及位于日韩、非洲和美洲扇区的地面磁站。通过将地面站的水平分量与磁层内的电分量和磁分量进行比较,我们报告了在 2017 年 9 月 6 日 12:02 UT 的 X9.3 级太阳耀斑抛射期间,从 12:05 UT 附近开始持续到 12:11 UT 的全球 Pi2。我们通过小波分析研究了垣冈(KAK)站和VAP-A卫星的Pi2振荡。通过分析高纬度台站,我们发现Pi2事件与极向边界强化(PBI)有很好的相关性。
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引用次数: 0
Resolved stellar populations as a key to unlocking the formation and evolution of galaxies 解析恒星群是开启星系形成和演化之门的钥匙
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-11-11 DOI: 10.1007/s10509-024-04376-6
Ata Sarajedini

We provide highlights of research investigations over the last five decades in the area of resolved stellar populations. After discussing the early work on the state of blue straggler stars in Galactic globular clusters, we broaden our gaze to include all of the stellar systems in the Local Volume with the overall goal of understanding the formation and evolution of galaxies. More specifically, we focus on the stellar constituents (e.g. star clusters and RR Lyrae variables) of the Milky Way, the Magellanic Clouds, the Andromeda galaxy (M31), the Triangulum galaxy (M33), as well as several dwarf galaxies in the Local Group and two dwarfs in the Sculptor group. Because of the available instrumental capabilities, work on resolved stars in galaxies has been largely focused on stellar systems in the Local Group and nearby galaxy groups. The big picture of galaxy formation and evolution that emerges from an analysis of all these constituents is largely consistent with the dwarf galaxy fragmentation and accretion scenario first put forth by Leonard Searle and Robert Zinn in 1978.

我们将重点介绍过去五十年来在解析恒星群领域的研究调查。在讨论了早期关于银河系球状星团中蓝色杂散恒星状态的工作之后,我们将目光扩大到包括本天体中的所有恒星系统,总体目标是了解星系的形成和演化。更具体地说,我们的研究重点是银河系、麦哲伦云、仙女座星系(M31)、三角座星系(M33)的恒星成分(如星团和天琴座RR变星),以及本星系群中的几个矮星系和雕刻星系群中的两个矮星系。由于现有的仪器能力,有关星系中解析恒星的工作主要集中在本星系群和附近星系群的恒星系统上。对所有这些成分的分析所得出的星系形成和演化的全貌,在很大程度上与 Leonard Searle 和 Robert Zinn 于 1978 年首次提出的矮星系碎裂和吸积设想是一致的。
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引用次数: 0
A real-time solar flare forecasting system with deep learning methods 采用深度学习方法的实时太阳耀斑预报系统
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-28 DOI: 10.1007/s10509-024-04374-8
Pengchao Yan, Xuebao Li, Yanfang Zheng, Liang Dong, Shuainan Yan, Shunhuang Zhang, Hongwei Ye, Xuefeng Li, Yongshang Lü, Yi Ling, Xusheng Huang, Yexin Pan

In this study, we develop five deep learning models, a Convolutional Neural Network (CNN) model, a CNN model with Squeeze-and-Excitation Attention(CNN-SE), a CNN model with Convolutional Block Attention Module (CNN-CBAM), a CNN model with Efficient Channel Attention (CNN-ECA), and a Vision Transformer (ViT) model, for predicting whether ≥C or ≥M-class solar flares occurring within 24 hours. We build a real-time forecasting system using these five models, which can achieve classification and probability forecasting. The 10-fold cross-validation sets are generated in chronological order using the full-disk magnetograms provided by the Solar Dynamics Observatory/Helioseismic and Magnetic Imager at 00:00 UT from May 1, 2010, to March 31, 2023. Then after training, validation, and testing our models, we compare the results with the true skill statistic (TSS) and Brier Skill Score (BSS) as assessment metrics. The major results are as follows: (1) There are no statistically significant differences in TSS and BSS performance between models with attention mechanisms and the CNN model. (2) For ≥C-class flare prediction, the Recall of the ViT model reaches 0.833, significantly better than that of the CNN model. For ≥M-class flare prediction, the Recall of the CNN-ECA and ViT models are 0.799 and 0.855, respectively, which are significantly higher than those of the CNN model. (3) We develop a full-disk solar flare prediction system that has been running since May 1, 2023. By December 31, all five models achieve a TSS of 0.984 for predicting ≥C-class flares, with the CNN-SE model demonstrating a BSS of 0.939. For ≥M-class flares, the CNN-SE model achieves a TSS of 0.304, while the BSS values for the CNN and CNN-SE models are 0.019 and 0.018, respectively. Additionally, the prediction performance for ≥M-class flares on the testing set without No-flare class samples, is similar to that of real-time predictions, validating the good generation performance of the model in real-time forecasting.

在本研究中,我们开发了五个深度学习模型,分别是卷积神经网络(CNN)模型、具有挤压和激发注意力(CNN-SE)的CNN模型、具有卷积块注意力模块(CNN-CBAM)的CNN模型、具有高效通道注意力(CNN-ECA)的CNN模型和视觉转换器(ViT)模型,用于预测24小时内发生的≥C级或≥M级太阳耀斑。我们利用这五个模型建立了一个实时预报系统,可以实现分类和概率预报。利用太阳动力学天文台/高地震和磁成像仪提供的从 2010 年 5 月 1 日至 2023 年 3 月 31 日 00:00 UT 的全磁盘磁图,按时间顺序生成 10 倍交叉验证集。然后,在对模型进行训练、验证和测试之后,我们将结果与真实技能统计量(TSS)和布赖尔技能得分(BSS)作为评估指标进行比较。主要结果如下(1) 具有注意力机制的模型与 CNN 模型在 TSS 和 BSS 性能上没有显著的统计学差异。(2)对于≥C 级耀斑预测,ViT 模型的 Recall 达到 0.833,明显优于 CNN 模型。对于≥M 级耀斑预测,CNN-ECA 模型和 ViT 模型的 Recall 分别为 0.799 和 0.855,明显高于 CNN 模型。(3) 我们开发的全盘太阳耀斑预测系统自 2023 年 5 月 1 日开始运行。到 12 月 31 日,五个模型预测≥C 级耀斑的 TSS 均达到 0.984,其中 CNN-SE 模型的 BSS 为 0.939。对于≥M 级耀斑,CNN-SE 模型的 TSS 值为 0.304,而 CNN 和 CNN-SE 模型的 BSS 值分别为 0.019 和 0.018。此外,在无耀斑类样本的测试集上,≥M 级耀斑的预测性能与实时预测性能相似,验证了该模型在实时预测中的良好生成性能。
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引用次数: 0
From TIGER to WST: scientific impact of four decades of developments in integral field spectroscopy 从 TIGER 到 WST:积分场光谱学四十年发展的科学影响
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-28 DOI: 10.1007/s10509-024-04369-5
Roland Bacon

This paper traces the 37 years of my career dedicated to the development of integral field spectroscopy (IFS), highlighting significant milestones and advancements. This extensive journey encompasses three generations of IFS: the initial prototype TIGER at CFHT, the first generation including OASIS at CFHT and SAURON at WHT, the second generation with MUSE at VLT, and the potential third generation represented by the Wide-field Spectroscopic Telescope (WST) project. Throughout, I discuss the lessons learned at each stage and provide my perspective on the future of IFS.

本文回顾了我 37 年来致力于发展积分场光谱学(IFS)的职业生涯,重点介绍了重要的里程碑和进展。这一漫长的历程涵盖了三代整体场光谱仪:CFHT 的最初原型 TIGER,包括 CFHT 的 OASIS 和 WHT 的 SAURON 在内的第一代,VLT 的 MUSE 在内的第二代,以及以宽视场光谱望远镜(WST)项目为代表的潜在第三代。在整个过程中,我讨论了每个阶段的经验教训,并对 IFS 的未来提出了自己的看法。
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引用次数: 0
Column fixed-pattern noise removal in solar images using two-way filtering 利用双向滤波去除太阳图像中的柱状固定模式噪声
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-25 DOI: 10.1007/s10509-024-04373-9
Hao Lin, Xianyong Bai, Song Feng, Bo Liang, Wenda Cao, Ding Yuan, Wei Dai, Yangfan Guo

Solar images are critically important for studying solar activities and features. Today, many observatories rely on CMOS sensors to acquire these images. However, these sensors often introduce column fixed-pattern noise (CFPN), seriously affecting image quality. Therefore, we proposed a two-way filtering algorithm to remove CFPN. Firstly, in the horizontal direction, we used the one-dimensional global weighted least squares filter and the efficient bilateral filter to obtain a coarse denoised image. Then, we utilized the weighted guided filter in the vertical direction to estimate the CFPN components, thereby obtaining a clean solar image. We selected three different solar observation images to compare and evaluate our results to those obtained by three comparative methods. The images are observed by the Solar Upper Transition Region Imager aboard the SATech-01 satellite. Additionally, we further used two quantitative metrics, photo response non-uniformity and mean relative deviation, to quantify the denoised results. The results demonstrate that our proposed method removes the CFPN better and preserves the image features in a more balanced way.

太阳图像对于研究太阳活动和特征至关重要。如今,许多天文台依靠 CMOS 传感器获取这些图像。然而,这些传感器经常会引入列固定模式噪声(CFPN),严重影响图像质量。因此,我们提出了一种去除 CFPN 的双向滤波算法。首先,在水平方向上,我们使用一维全局加权最小二乘法滤波器和高效双边滤波器获得粗去噪图像。然后,我们利用垂直方向上的加权导向滤波器来估计 CFPN 成分,从而获得干净的太阳图像。我们选择了三幅不同的太阳观测图像,将我们的结果与三种比较方法获得的结果进行比较和评估。这些图像是由 SATech-01 卫星上的太阳上过渡区成像仪观测到的。此外,我们还进一步使用了两个量化指标,即光反应不均匀性和平均相对偏差,来量化去噪结果。结果表明,我们提出的方法能更好地去除 CFPN,并以更均衡的方式保留图像特征。
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引用次数: 0
Ionospheric response to the 08 April 2024 total solar eclipse over United States: a case study 电离层对 2024 年 4 月 8 日美国上空日全食的响应:案例研究
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-24 DOI: 10.1007/s10509-024-04372-w
Sujan Prasad Gautam, Atirsaw Muluye Tilahun, Ashok Silwal, Binod Adhikari, Yohannes Getachew Ejigu

A total solar eclipse occurred on April 8, 2024, across the United States, with obscuration rates ranging from 20–100% at different locations. We study the ionospheric Total Electron Content (TEC) response to the eclipse using data from 51 ground-based GPS stations. We find a significant depletion in TEC of up to 65%, with larger depletion rates occurring along the path of totality. We also observe a time delay between the maximum TEC depletion and the time of maximum obscuration, ranging from 8 to 80 minutes, with longer delays occurring at stations with lower obscuration rates. Both time delay and TEC depletion rates are found to vary with latitude, with slightly longer delays at lower latitudes and higher TEC depletion rates at mid-latitudes. The TEC depletion rate also increased with local time, showing a higher decrement after noon compared to before. The spatiotemporal variation in TEC closely followed the eclipse’s path, indicating a positive correlation with the movement of the moon’s shadow. Monitoring rate of TEC change during such rare events is crucial for enhancing our understanding of ionospheric dynamics, which can be very helpful to improve the accuracy of global communication and navigation systems.

2024 年 4 月 8 日,美国各地发生了日全食,不同地点的遮蔽率从 20% 到 100% 不等。我们利用 51 个地面 GPS 站的数据研究了电离层电子总含量(TEC)对日全食的响应。我们发现电离层电子总含量(TEC)有明显下降,最高可达 65%,全食路径沿线的下降率更大。我们还观察到最大 TEC 损耗时间与最大遮挡时间之间存在时间延迟,从 8 分钟到 80 分钟不等,遮挡率较低的站点出现的时间延迟更长。时间延迟和 TEC 耗损率都随纬度的变化而变化,低纬度地区的时间延迟稍长,而中纬度地区的 TEC 耗损率较高。TEC 耗损率也随当地时间的变化而增加,正午之后的耗损率比正午之前要高。熱釋光的時空變化緊貼月食的路徑,顯示與月影的移動呈正相關。在这种罕见事件中监测 TEC 的变化率对加强我们对电离层动态的了解至关重要,这对提高全球通信和导航系统的准确性非常有帮助。
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引用次数: 0
Unified model of blazars and radio galaxies: synthesizing observational data with relativistic beaming theory 耀斑和射电星系的统一模型:将观测数据与相对论光束理论综合起来
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-22 DOI: 10.1007/s10509-024-04371-x
E. U. Iyida, C. I. Onah, I. O. Eya, F. C. Odo

The unified model of jetted active galactic nuclei (AGNs) based on intrinsic properties presumes that the blazar subtypes of BL Lacertae objects (BLs) and flat-spectrum radio quasars (FSRQs) are aligned equivalents of Fanaroff–Riley type I (FR I) and Fanaroff–Riley type II (FR II) radio galaxies (RGs) from where their parent sources are obtained. Using compiled radio, X-ray and (gamma )-ray data of 397 Fermi Large Area Telescope (Fermi-LAT) blazars and 153 non-Fermi detected RGs, we computed the (gamma )-ray core-dominance parameter (Rγ) and (gamma )-ray emission components (beamed and unbeamed) to study the consequences of relativistic beaming and orientation effects on (gamma )-ray properties of radio RGs, BLs and FSRQs. Data analysis shows that the distributions of RX and Rγ, on average, are consistent with the prediction of the unified scheme in which FSRQs and BLs are strongly beamed and inclined at smaller angles than RGs. Through statistical tests with chance probability, (p < 0.05), we find that the distributions of RX and Rγ for radio galaxies and the blazar subtypes are not significantly different. There is a regular positive trend ((r > +0.60)) in the variation of radio core-dominance parameter – X-ray luminosity ((R - L_{mathrm{x}})) data from radio galaxies to FSRQs through BLs, which suggests that radio galaxies could be relativistically less beamed population of jetted AGNs. The results are consistent with the unified model for radio galaxies and the conventional blazar subtypes.

基于固有特性的喷射活动星系核(AGNs)统一模型假定,BL Lacertae天体(BLs)和平谱射电类星体(FSRQs)的耀星亚型是Fanaroff-Riley I型(FR I)和Fanaroff-Riley II型(FR II)射电星系(RGs)的对齐等价物,而它们的母源就是从RGs中获得的。利用汇编的397个费米大面积望远镜(Fermi-LAT)blazars和153个非费米探测到的RGs的射电、X射线和(γ)射线数据,我们计算了它们的((γ))等效值、我们计算了射电RGs、BLs和FSRQs的(gamma)-射线核心主导参数(Rγ)和(gamma)-射线发射成分(束射和非束射),以研究相对论束射和定向效应对射电RGs、BLs和FSRQs的(gamma)-射线特性的影响。数据分析显示,RX和Rγ的平均分布与统一方案的预言一致,即FSRQs和BLs比RGs受到强束流,并且倾斜角度更小。通过概率统计检验(p <0.05),我们发现射电星系的RX和Rγ的分布与耀斑亚型没有显著差异。射电核心主导参数-X射线光度(R-L_{mathrm{x}}/)数据从射电星系到FSRQs再到BLs的变化存在一个有规律的正趋势((r > +0.60)),这表明射电星系可能是相对论上较少束流的喷流AGN群。这些结果与射电星系的统一模型和传统的耀星亚型是一致的。
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引用次数: 0
On the mass assembly history of the Milky Way: clues from its stellar halo 论银河系的质量集合史:来自其恒星晕的线索
IF 1.8 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2024-10-22 DOI: 10.1007/s10509-024-04370-y
Danny Horta, Ricardo P. Schiavon

Stellar halos of galaxies retain crucial clues to their mass assembly history. It is in these galactic components that the remains of cannibalised galactic building blocks are deposited. For the case of the Milky Way, the opportunity to analyse the stellar halo’s structure on a star-by-star basis in a multi-faceted approach provides a basis from which to infer its past and assembly history in unrivalled detail. Moreover, the insights that can be gained about the formation of the Galaxy not only help constrain the evolution of our Milky Way, but may also help place constraints on the formation of other disc galaxies in the Universe. This paper includes a summary of work undertaken during a PhD thesis aiming to make progress toward answering the most fundamental question in the field of Galactic archaeology: “How did the Milky Way form?” Through the effort to answer this question, we summarise new insights into aspects of the history of assembly and evolution of our Galaxy and measurements of the structure of various of its Galactic components.

星系的恒星晕保留了其质量组装历史的重要线索。正是在这些星系组成部分中,沉积着被分解的星系构件的残骸。就银河系而言,通过多角度方法逐星分析恒星晕结构的机会,为推断其过去和组装历史提供了无与伦比的详细基础。此外,对银河系形成过程的深入了解不仅有助于制约银河系的演化,还可能有助于制约宇宙中其他圆盘星系的形成。本文是一篇博士论文的摘要,旨在回答银河系考古学领域最基本的问题:"银河系是如何形成的?通过回答这个问题,我们总结了对银河系的组装和演化历史的新见解,以及对银河系各组成部分结构的测量结果。
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引用次数: 0
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