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Archaeoastronomy and Cognition: La Mink'a and La Mit'a From the Logic of Relations's Perspective 考古天文学与认知:关系逻辑视角下的“Mink’a”与“La Mit’a”
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-05-07 DOI: 10.1002/asna.70001
Mônica Estrázulas

To understand the contributions of ancient civilizations to the evolution of knowledge in the fields of archaeoastronomy and/or science in general, through a cognitive perspective, we seek to identify conceptual elements that are consonant and converge with science. All of them come from a cognitive processes in which the subject and the object of knowledge collaborate in a progressive constitution, according to Genetic Epistemology. It is necessary to identify the presence of logic as a mental structure that allows the subject to be capable of supporting the scientific work. In this article, we analyze dates that come from the inca's concept of Ayni which permeates the activities La Mint'a and La Mink'a and demonstrates the presence of the same cognitive structure—the logical—required by scientific work.

为了从认知的角度理解古代文明对考古天文学和/或一般科学领域知识发展的贡献,我们试图找出与科学一致并趋于一致的概念要素。根据遗传认识论,所有这些都来自一个认知过程,在这个过程中,知识的主体和客体在一个渐进的结构中合作。有必要确定逻辑的存在是一种心理结构,它允许主体能够支持科学工作。在这篇文章中,我们分析了来自印加人的Ayni概念的日期,它渗透到La Mint'a和La Mink'a的活动中,并证明了科学工作所需的相同认知结构-逻辑的存在。
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引用次数: 0
Gaia Search for Stellar Companions of TESS Objects of Interest V 盖亚搜寻TESS感兴趣的伴星V
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-05-01 DOI: 10.1002/asna.70005
Markus Mugrauer, Ann-Kathrin Kollak, Lara Pietsch, Kai-Uwe Michel

In this paper, we present the latest results of our ongoing multiplicity survey of (Community) TESS Objects of Interest, using astrometry and photometry from the latest data release of the ESA Gaia mission to detect stellar companions of these stars and to characterize their properties. A total of 92 binary and two hierarchical triple star systems are identified among the 745 target stars whose multiplicity is explored in this study, all at distances of less than 500 pc around the Sun. As expected for components of gravitationally bound star systems, the targets and the detected companions are at the same distance and share a common proper motion, as shown by their accurate Gaia astrometry. The companions have masses of about 0.12 to 1.6 M$$ {M}_{odot } $$ and are most frequently found in the mass range up to 0.6 M$$ {M}_{odot } $$. The companions have projected separations from the targets between about 110 and 9600 au. Their frequency is highest and constant from about 300 to 800 au, decreasing at larger projected separations. In addition to main sequence stars, five white dwarf companions are detected in this study, whose true nature is unveiled by their photometric properties.

在本文中,我们介绍了我们正在进行的(社区)TESS感兴趣对象的多重调查的最新结果,使用欧空局盖亚任务最新数据发布的天体测量学和光度学来探测这些恒星的恒星伴星并表征它们的特性。在本次研究中探索的745颗目标恒星中,共有92颗双星和2颗分层三星系统被确定,所有这些恒星的距离都小于太阳周围500倍。正如对引力束缚恒星系统的组成部分所期望的那样,目标和被探测到的伴星处于相同的距离,并有共同的固有运动,正如它们精确的盖亚天体测量所显示的那样。伴星的质量约为0.12至1.6 M⊙$$ {M}_{odot } $$,最常发现的质量范围高达0.6 M⊙$$ {M}_{odot } $$。伴星预计与目标的距离在110至9600天文单位之间。它们的频率最高,在大约300到800 au之间保持不变,在较大的投影距离处下降。除了主序星外,本研究还发现了五颗白矮星伴星,它们的光度特性揭示了它们的真实性质。
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引用次数: 0
Compressibility Function and Speed of Sound in the Non-Commutative Quantum Hadrodynamics Type-I Model for Neutron Stars 中子星非交换量子流体动力学i型模型中的压缩函数和声速
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-05-01 DOI: 10.1002/asna.70008
João Gabriel Galli Gimenez, Dimiter Hadjimichef, César A. Zen Vasconcellos

We investigate the effects of a minimal measurable length on neutron stars, within the quantum hadrodynamics (QHD-I) model modified by the Generalized Uncertainty Principle (GUP). Working in a deformed Poisson algebra framework, we incorporate GUP effects via a time-invariant transformation of the phase space volume, effectively reducing the number of accessible quantum states at high momentum. We focus specifically on two observables critical to this star physics, the compressibility, which encapsulates how stiff EOS become, and the speed of sound, which imposes a causality constraint. Using this model as an exploratory study, due to its simplicity and structured description, we perform a preliminary analysis of GUP effects with a minimum spacetime length on these compact objects. This deformation increases the speed of sound while decreasing the compressibility, and we identify critical values of the Fermi momentum beyond which both quantities become nonphysical. These results underscore the potential role of a minimal length scale in shaping the bulk properties and possible phase structures of dense matter in neutron stars.

我们在广义不确定性原理(GUP)修正的量子流体动力学(QHD-I)模型中研究了最小可测量长度对中子星的影响。在一个变形的泊松代数框架中,我们通过相空间体积的时不变变换来结合GUP效应,有效地减少了高动量下可访问量子态的数量。我们特别关注对这颗恒星物理至关重要的两个可观测值,压缩性,它封装了EOS变得有多硬,以及声速,它施加了因果关系约束。利用该模型作为探索性研究,由于其简单和结构化的描述,我们对这些致密物体在最小时空长度下的GUP效应进行了初步分析。这种变形增加了声速,同时降低了可压缩性,我们确定了费米动量的临界值,超过这个临界值,两个量都变得非物理。这些结果强调了最小长度尺度在塑造中子星致密物质的体积特性和可能的相结构方面的潜在作用。
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引用次数: 0
Dark Energy From the Gravitational Wave Background With Scalar Field Dark Matter 引力波背景暗能量与标量场暗物质
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-04-22 DOI: 10.1002/asna.70004
Edwin L. Pérez-Ochoa, Tonatiuh Matos

Recent observational results, such as those from pulsar timing arrays (PTA), suggest a low-frequency Gravitational Wave Background (GWB) permeates our universe. This opens the possibility that gravitational waves could span a broader spectrum, potentially impacting cosmological scales. Among novel Dark Energy (DE) models that explain DE as a very low-frequency GWB, the Compton Mass Dark Energy model (CMaDE) has shown promising theoretical alignment with cosmic acceleration. In this study, we explore the cosmological implications of the CMaDE model when coupled with Scalar Field Dark Matter (SFDM) as the dark matter candidate. We numerically solve the cosmological evolution equations for this combined CMaDE+SFDM framework, examining its impact on key observables and comparing results to the standard ΛCDM$$ Lambda mathrm{CDM} $$ model. Our findings demonstrate that the CMaDE+SFDM model is broadly consistent with ΛCDM$$ Lambda mathrm{CDM} $$, showing similar evolution in observables such as the cosmic microwave background and the background energy densities, with some deviations that merit further investigation.

最近的观测结果,如脉冲星定时阵列(PTA)的观测结果,表明低频引力波背景(GWB)弥漫在我们的宇宙中。这开启了引力波可能跨越更广泛的频谱,潜在地影响宇宙尺度的可能性。在新的暗能量(DE)模型中,将DE解释为非常低频的GWB,康普顿质量暗能量模型(cmake)显示出与宇宙加速有希望的理论一致性。在这项研究中,我们探索了cmake模型与标量场暗物质(SFDM)作为暗物质候选者耦合时的宇宙学意义。我们对这个cmake +SFDM组合框架的宇宙学演化方程进行了数值求解,考察了其对关键观测值的影响,并将结果与标准ΛCDM $$ Lambda mathrm{CDM} $$模型进行了比较。我们的研究结果表明,cmake +SFDM模型与ΛCDM $$ Lambda mathrm{CDM} $$大致一致,在宇宙微波背景和背景能量密度等可观测数据中显示出类似的演化,但存在一些偏差,值得进一步研究。
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引用次数: 0
The Quest for the Quark-Gluon Plasma From the Perspective of Dynamical Models of Relativistic Heavy-Ion Collisions 从相对论性重离子碰撞动力学模型的角度探索夸克-胶子等离子体
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-04-10 DOI: 10.1002/asna.70006
Marcus Bleicher, Elena Bratkovskaya

The physics of heavy-ion collisions is one of the most exciting and challenging directions of science for the last four decades. On the theoretical side one deals with a non-abelian field theory, while on the experimental side today's largest accelerators are needed to enable these studies. The discovery of a new stage of matter—called the quark-gluon plasma (QGP) - and the study of its properties is one of the major achievements of modern physics. In this contribution we briefly review the history of theoretical descriptions of heavy-ion collisions based on dynamical models, focusing on the personal experiences in this inspiring field.

重离子碰撞物理学是过去四十年来最令人兴奋和最具挑战性的科学方向之一。在理论方面,人们处理非阿贝尔场论,而在实验方面,今天最大的加速器需要实现这些研究。物质的新阶段——夸克-胶子等离子体(QGP)的发现及其性质的研究是现代物理学的主要成就之一。在这篇文章中,我们简要回顾了基于动力学模型的重离子碰撞理论描述的历史,重点介绍了在这个鼓舞人心的领域的个人经历。
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引用次数: 0
Glueball-Like Decay of X(1835) Into Two Photons X(1835)的类胶球衰变为两个光子
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-04-04 DOI: 10.1002/asna.20250030
D. T. Da Silva, M. L. L. Da Silva
<div> <p>The search for new states of matter has been the subject of study and research, as well as their identification in colliders, with exotic states being identified in experiments around the world in recent years. Among the possible exotic states provided in QCD we have the glueball, a bound state between gluons. Using a non-relativistic gluon bound state model, we calculate <span></span><math> <semantics> <mrow> <mi>Γ</mi> <mrow> <mo>(</mo> <mrow> <mi>G</mi> <mo>→</mo> <mrow> <mi>γ</mi> <mi>γ</mi> </mrow> </mrow> <mo>)</mo> </mrow> </mrow> <annotation>$$ Gamma left(Gto gamma gamma right) $$</annotation> </semantics></math>, where <span></span><math> <semantics> <mrow> <mi>G</mi> </mrow> <annotation>$$ G $$</annotation> </semantics></math> is a pseudoscalar digluon (<span></span><math> <semantics> <mrow> <msup> <mn>0</mn> <mrow> <mo>−</mo> <mo>+</mo> </mrow> </msup> </mrow> <annotation>$$ {0}^{-+} $$</annotation> </semantics></math>), which is applied to a possible exotic state, the meson <span></span><math> <semantics> <mrow> <mi>X</mi> <mrow> <mo>(</mo> <mn>1835</mn> <mo>)</mo> </mrow> </mrow> <annotation>$$ X(1835) $$</annotation> </semantics></math>. We start from the amplitudes, where we consider the process <span></span><math> <semantics> <mrow> <mrow> <mi>γ</mi> <mi>γ</mi> </mrow> <mo>→</mo> <msup> <mi>g</mi> <mo>*</mo> </msup> <msup> <mi>g</mi> <mo>*</mo> </msup> </mrow> <annotation>$$ gamma gamma to {g}^{ast }{g}^{ast } $$</annotation> </semantics></math>, with the <i>g</i>*s being the massive constituent gluons and the amplitudes obtained in the lowest-order perturbative QCD deriving them from the QED calculation. The unknown parameters of the model such as the digluon wavefunction are obtained using experimentally measured values of the decay of <span></span><math>
寻找物质的新状态一直是研究和研究的主题,在对撞机中识别它们也是如此,近年来在世界各地的实验中发现了奇异的状态。在QCD提供的可能的奇异态中,我们有胶球,胶子之间的束缚态。使用非相对论胶子束缚态模型,我们计算Γ (G→Γ Γ) $$ Gamma left(Gto gamma gamma right) $$,其中G $$ G $$是一个伪标量双子(0−+ $$ {0}^{-+} $$),它被应用于一个可能的奇异态,介子X (1835) $$ X(1835) $$。我们从振幅开始,考虑过程γ γ→g * g * $$ gamma gamma to {g}^{ast }{g}^{ast } $$,其中g*s是大质量的组成胶子,而在最低阶微扰QCD中得到的振幅是由QED计算得出的。利用Γ (J / Ψ→G Γ)衰变的实验测量值获得了模型的未知参数,如狄光子波函数。$$ Gamma left(J/Psi to Ggamma right) $$。我们将我们的理论结果与我们的胶球候选物X (1835) $$ X(1835) $$的当前实验极限进行了比较。
{"title":"Glueball-Like Decay of X(1835) Into Two Photons","authors":"D. T. Da Silva,&nbsp;M. L. L. Da Silva","doi":"10.1002/asna.20250030","DOIUrl":"https://doi.org/10.1002/asna.20250030","url":null,"abstract":"&lt;div&gt;\u0000 \u0000 &lt;p&gt;The search for new states of matter has been the subject of study and research, as well as their identification in colliders, with exotic states being identified in experiments around the world in recent years. Among the possible exotic states provided in QCD we have the glueball, a bound state between gluons. Using a non-relativistic gluon bound state model, we calculate &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;Γ&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;(&lt;/mo&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;G&lt;/mi&gt;\u0000 &lt;mo&gt;→&lt;/mo&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;γ&lt;/mi&gt;\u0000 &lt;mi&gt;γ&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;)&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ Gamma left(Gto gamma gamma right) $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;, where &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;G&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ G $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt; is a pseudoscalar digluon (&lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;msup&gt;\u0000 &lt;mn&gt;0&lt;/mn&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;−&lt;/mo&gt;\u0000 &lt;mo&gt;+&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ {0}^{-+} $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;), which is applied to a possible exotic state, the meson &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;X&lt;/mi&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mo&gt;(&lt;/mo&gt;\u0000 &lt;mn&gt;1835&lt;/mn&gt;\u0000 &lt;mo&gt;)&lt;/mo&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ X(1835) $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;. We start from the amplitudes, where we consider the process &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 &lt;semantics&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mrow&gt;\u0000 &lt;mi&gt;γ&lt;/mi&gt;\u0000 &lt;mi&gt;γ&lt;/mi&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;mo&gt;→&lt;/mo&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;g&lt;/mi&gt;\u0000 &lt;mo&gt;*&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;msup&gt;\u0000 &lt;mi&gt;g&lt;/mi&gt;\u0000 &lt;mo&gt;*&lt;/mo&gt;\u0000 &lt;/msup&gt;\u0000 &lt;/mrow&gt;\u0000 &lt;annotation&gt;$$ gamma gamma to {g}^{ast }{g}^{ast } $$&lt;/annotation&gt;\u0000 &lt;/semantics&gt;&lt;/math&gt;, with the &lt;i&gt;g&lt;/i&gt;*s being the massive constituent gluons and the amplitudes obtained in the lowest-order perturbative QCD deriving them from the QED calculation. The unknown parameters of the model such as the digluon wavefunction are obtained using experimentally measured values of the decay of &lt;span&gt;&lt;/span&gt;&lt;math&gt;\u0000 ","PeriodicalId":55442,"journal":{"name":"Astronomische Nachrichten","volume":"346 3-4","pages":""},"PeriodicalIF":1.1,"publicationDate":"2025-04-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"144206442","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 0
A Slowly Pulsating Run-Away B Star at High Galactic Latitude Ejected From a Spiral Arm 在银河系高纬度处,一颗缓慢脉动的逃逸B星从旋臂中喷射出来
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-04-04 DOI: 10.1002/asna.70003
Ulrich Heber, Maximilian Halenke, Aakash Bhat, Veronika Schaffenroth

We report the discovery of the young B6 V run-away star LAMOST J083323.18 + 430825.4, 2.5 kpc above the Galactic plane. Its atmospheric parameters and chemical composition are determined from LAMOST spectra, indicating normal composition. Effective temperature (Teff$$ {T}_{mathrm{eff}} $$ = 14,500$$ mathrm{14,500} $$ K) and gravity (logg$$ log g $$ = 3.79$$ 3.79 $$) suggest that the star is close to terminating hydrogen burning. An analysis of the spectral energy distribution allowed us to determine the angular diameter as well as the interstellar reddening. Using evolutionary models from the MIST database we derived the stellar mass (4.75M$$ 4.75{M}_{odot } $$) and age (10413+11$$ {104}_{-13}^{+11} $$ Myr). The spectroscopic distance (4.17 kpc), the radius (4.5R$$ 4.5{R}_{odot } $$), and the luminosity (<

我们报告在银道平面上方2.5 kpc处发现了年轻的B6 V逃逸恒星LAMOST J083323.18 + 430825.4。根据LAMOST光谱测定了其大气参数和化学成分,表明其成分正常。有效温度(T eff $$ {T}_{mathrm{eff}} $$ = 14,500 $$ mathrm{14,500} $$ K)和重力(log g $$ log g $$)= 3.79 $$ 3.79 $$)表明这颗恒星已经接近氢燃烧的终点。对光谱能量分布的分析使我们能够确定角直径以及星际变红。利用MIST数据库中的演化模型,我们得到了恒星质量(4.75 M⊙$$ 4.75{M}_{odot } $$)和年龄(104−13)+ 11 $$ {104}_{-13}^{+11} $$ Myr)。光谱距离(4.17 kpc),半径(4.5 R⊙$$ 4.5{R}_{odot } $$)光度(log L / L⊙$$ log left(L/{L}_{odot}right) $$ = 2.89$$ 2.89 $$),然后由大气参数得出。利用盖亚固有运动,轨迹可以追溯到银河系盘,以确定螺旋臂中的出生地点。92 km s−1的弹射速度是典型的逃逸恒星在光晕中的速度。这颗恒星的年龄大于它的飞行时间(78±4 $$ 78pm 4 $$ Myr),这有利于双超新星事件作为可能的弹射机制。TESS的光曲线显示出3.58天周期的变化,由此我们得出结论,它是一颗缓慢脉动的b星,是已知的极少数会脉动的逃逸b星之一。
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引用次数: 0
Modified Field Equation With Gauss–Bonnet Gravity 高斯- bonnet重力下的修正场方程
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-03-26 DOI: 10.1002/asna.20250027
Zhi-Fu Gao, Xin-Jun Zhao, Xiao-Feng Yang, Wen-Qi Ma, Zi-Rui Hu

This work provides a comprehensive analysis of modifications to the Einstein–Hilbert action, with a particular focus on Gauss–Bonnet (GB) gravity, and addresses the theoretical challenges in unifying quantum gravity frameworks with the GB gravitational modifications. By developing a novel fourth-order tensor methodology to manage derivative couplings, we establish a stable framework that eliminates higher-order derivative instabilities while enabling modified gravitational phenomena. The model maintains consistency with low-energy string theory constraints and generates testable predictions for black hole thermodynamics and cosmic expansion dynamics. Our results reconcile discrepancies between modified gravity theories and quantum field theory requirements, providing new mathematical tools for analyzing high-energy gravitational interactions. This work bridges critical gaps between theoretical formulations and observational evidence in cosmology, offering a unified approach to modeling gravitational interactions across quantum and cosmological scales.

这项工作提供了对爱因斯坦-希尔伯特作用的修正的全面分析,特别关注高斯-邦尼特(GB)引力,并解决了统一量子引力框架与GB引力修正的理论挑战。通过开发一种新的四阶张量方法来管理导数耦合,我们建立了一个稳定的框架,消除了高阶导数的不稳定性,同时实现了修正的引力现象。该模型保持了低能量弦理论约束的一致性,并对黑洞热力学和宇宙膨胀动力学产生了可测试的预测。我们的结果调和了修正引力理论与量子场论要求之间的差异,为分析高能引力相互作用提供了新的数学工具。这项工作弥合了宇宙学理论公式和观测证据之间的关键差距,提供了一种统一的方法来模拟量子和宇宙尺度上的引力相互作用。
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引用次数: 0
Preface to the 11th International Workshop on Astronomy and Relativistic Astrophysics (IWARA 2024) 第11届天文学与相对论天体物理学国际研讨会(IWARA 2024)序言
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-03-25 DOI: 10.1002/asna.20250042
César Augusto Zen Vasconcellos, Peter Hess, Fridolin Weber, Remo Ruffini, Jorge Horvath, Zhifu Gao, Dimiter Hadjimichef, Benno Bodmann

This Conference Proceedings volume contains the written versions of most of the contributions presented during the 11th International Workshop on Astronomy and Relativistic Astrophysics (IWARA 2024). The Workshop took place in Machupicchu Pueblo (Aguas Calientes), Peru, from September 2–6, 2024. The Workshop provided a setting for discussing recent developments in a wide variety of topics, including Archaeoastronomy and Cognition, the Kerr metric and the Hawking temperature, Damour-Solodukhin-type Wormholes, Stellar Physics and General Relativity, Stochastic Quantum Mechanics in Curved Spaces, Gauss-Bonnet Theory, Quantum Gravity, Black Holes, Fast Radio Bursts, Neutron Stars, Strange Stars, X-ray Binaries, Pulsars, Gravitational Waves, and Dark Matter, among others. Most of these contributions are included in this volume.

本会议论文集收录了第11届国际天文学和相对论天体物理学研讨会(IWARA 2024)期间发表的大部分论文的书面版本。研讨会于2024年9月2日至6日在秘鲁马丘比丘普韦布洛(阿瓜斯卡连特斯)举行。研讨会提供了一个讨论各种主题的最新发展的环境,包括考古天文学和认知,克尔度量和霍金温度,damur - solodukhin型虫洞,恒星物理学和广义相对论,弯曲空间中的随机量子力学,高斯-邦纳理论,量子引力,黑洞,快速射电暴,中子星,奇异星,x射线双星,脉冲星,引力波和暗物质等。这些贡献中的大部分都包含在本卷中。
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引用次数: 0
Estimating the Spin of MAXI J1820+070 From Soft State by Insight-HXMT 用Insight-HXMT从软态估计MAXI J1820+070的自旋
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-03-25 DOI: 10.1002/asna.20250021
Chun-Xiang Liao, Chao Huang, Jian-Chao Feng, Ai-Jun Dong

MAXI J1820+070, discovered by the Monitor of All-sky X-ray Image (MAXI) in 2018, is a well-known black hole X-ray binary. This study presents a detailed spectral analysis using 2018 observations from the Insight Hard X-ray Modulation Telescope (HXMT). We explored the evolution of the Fe line shape and found it stable at 6.4 keV in the high/soft state, indicating the inner radius of the accretion disk remains at the Innermost Stable Circular Orbit. Additionally, we estimated the black hole spin (a*$$ {a}_{ast } $$) using the continuum fitting method, obtaining a spin of a*=0.1220.016+0.013$$ {a}_{ast }={0.122}_{-0.016}^{+0.013} $$, consistent with previous results. Through these findings, this study has contributed to the spectral analysis and spin parameter estimation of black hole X-ray binary systems, offering valuable insights into black hole behavior and its role in cosmology.

MAXI J1820+070是由全天x射线图像监视器(MAXI)于2018年发现的,是一个著名的黑洞x射线双星。本研究利用洞察号硬x射线调制望远镜(HXMT) 2018年的观测数据进行了详细的光谱分析。我们探索了铁线形状的演变,发现它在高/软状态下稳定在6.4 keV,表明吸积盘的内半径保持在最内层稳定圆轨道。此外,我们使用连续统拟合方法估计了黑洞自旋(a * $$ {a}_{ast } $$),得到自旋a * = 0.122−0.016 + 0.013 $$ {a}_{ast }={0.122}_{-0.016}^{+0.013} $$,与之前的结果一致。通过这些发现,本研究为黑洞x射线双星系统的光谱分析和自旋参数估计做出了贡献,为黑洞行为及其在宇宙学中的作用提供了有价值的见解。
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Astronomische Nachrichten
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