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Investigating the Evolution of Compact Object Populations 研究紧凑天体种群的演化
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-24 DOI: 10.1002/asna.20250018
J. E. Horvath, L. M. de Sá, L. S. Rocha, N. D. Pires, R. Miwa, D. Rodrigues, L. G. Barão, G. Y. Chinen, The GARDEL Group

The population of compact objects both Galactic and extragalactic can now be studied and verified observationally with increasing efficiency, the latter thanks to the detection of compact object mergers through gravitational waves. The formation channels of merging compact object binaries are, however, not yet fully understood, and may even vary over cosmic time. We address this problem with a population synthesis approach, including BOSSA, a new initial sampling code, to deal with the variation of initial conditions and evaluate its consequences.

银河系和星系外致密天体的数量现在可以通过观测来研究和验证,效率越来越高,后者要归功于通过引力波探测致密天体合并。然而,合并致密双星的形成通道尚未完全被理解,甚至可能随着宇宙时间的推移而变化。我们用包括BOSSA(一种新的初始抽样代码)在内的总体综合方法来解决这个问题,以处理初始条件的变化并评估其后果。
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引用次数: 0
A Simplified Bead-on-Wire Model With Relativistic Revision for Magnetized Outflow 磁化流出流的简化磁珠线上模型及相对论修正
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-20 DOI: 10.1002/asna.20250019
Wei Xie, Zi-Ru He

Outflows are ubiquitous in various astrophysical objects, yet the mechanism responsible for generating outflows remains unclear. One possibility is that outflows are driven by large-scale magnetic fields. When dealing with magnetically driven outflows, the one-dimensional model proposed by Weber and Davis in 1967 is often employed. However, as it was originally a non-relativistic theory, this limits its application in high-energy astrophysical scenarios. This work attempts to modify the non-relativistic Bernoulli equation into its relativistic form through an analogy method, thereby applying it to relativistic outflows and comparing the results with those of classical theory. We find that when the initial temperature of the outflow is sufficiently high or when the angular velocity of rotation of the magnetic field lines is sufficiently fast, the terminal velocity of the outflow can be relativistic. The relativistically modified Bernoulli equation established in this paper could be conveniently applied in the context of extremely high-velocity outflows from different sources.

喷流在各种天体中无处不在,但产生喷流的机制尚不清楚。一种可能性是,外流是由大规模磁场驱动的。在处理磁驱动外流时,通常采用韦伯和戴维斯在1967年提出的一维模型。然而,由于它最初是一个非相对论理论,这限制了它在高能天体物理场景中的应用。本文试图通过类比方法将非相对论伯努利方程修正为相对论形式,从而将其应用于相对论外流,并将结果与经典理论的结果进行比较。我们发现,当出口的初始温度足够高或当磁力线的旋转角速度足够快时,出口的终端速度可以是相对论性的。本文建立的相对论修正伯努利方程可以方便地应用于不同来源的极高速度流出。
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引用次数: 0
Holographic Connection of f(G) Gravity Through Barrow and a Generalized Version of Holographic Dark Fluid f(G)引力通过Barrow的全息连接和全息暗流体的广义版本
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-20 DOI: 10.1002/asna.20240149
Surajit Chattopadhyay
<div> <p>In the study presented in this work, we use the holographic principle taking into account the Barrow entropy rather than the conventional Bekenstein–Hawking one to develop a holographic model for dark energy in the <span></span><math> <semantics> <mrow> <mi>f</mi> <mrow> <mo>(</mo> <mi>G</mi> <mo>)</mo> </mrow> </mrow> <annotation>$$ f(G) $$</annotation> </semantics></math> gravity. The former results from the attempt to include quantum gravitational effects into the cosmological framework and, in accordance with the gravity–thermodynamic conjecture, into black hole physics. To investigate the cosmological implications of our model for <span></span><math> <semantics> <mrow> <mi>f</mi> <mrow> <mo>(</mo> <mi>G</mi> <mo>)</mo> </mrow> </mrow> <annotation>$$ f(G) $$</annotation> </semantics></math> modified gravity, we discuss the cosmic implementation of the most generalized type of holographic dark energy, called Nojiri-Odintsov holographic dark energy (NO-HDE), and a particular example of it, called Barrow holographic dark energy. This is accomplished by adding to the <span></span><math> <semantics> <mrow> <mi>f</mi> <mrow> <mo>(</mo> <mi>G</mi> <mo>)</mo> </mrow> </mrow> <annotation>$$ f(G) $$</annotation> </semantics></math> model a well-known power law form of the scale factor <span></span><math> <semantics> <mrow> <mi>a</mi> <mrow> <mo>(</mo> <mi>t</mi> <mo>)</mo> </mrow> </mrow> <annotation>$$ a(t) $$</annotation> </semantics></math> and the Holographic dark energy. It is found that the reconstructed <span></span><math> <semantics> <mrow> <mi>f</mi> <mrow> <mo>(</mo> <mi>G</mi> <mo>)</mo> </mrow> </mrow> <annotation>$$ f(G) $$</annotation> </semantics></math> satisfies a necessary condition for a realistic modified gravity model. Additionally, the reconstruction models are examined in the four energy scenarios. Lastly, the relationship to observational boundaries is examined, and the reconstructed EoS parameter is verified to fall within the constraints determined in the literature by utilizing observat
在这项工作中提出的研究中,我们使用了考虑巴罗熵而不是传统的贝肯斯坦-霍金熵的全息原理来开发f (G) $$ f(G) $$重力下暗能量的全息模型。前者源于试图将量子引力效应纳入宇宙学框架,并根据引力-热力学猜想纳入黑洞物理学。为了研究f (G) $$ f(G) $$修正引力模型的宇宙学含义,我们讨论了最广义的全息暗能量类型的宇宙实现,称为nojri - odintsov全息暗能量(NO-HDE),以及它的一个特殊例子。叫做巴罗全息暗能量。这是通过在f (G) $$ f(G) $$模型中加入众所周知的比例因子a (t) $$ a(t) $$的幂律形式来实现的以及全息暗能量。发现重建的f (G) $$ f(G) $$满足一个真实修正重力模型的必要条件。此外,还对四种能源情景下的重建模型进行了检验。最后,利用BAO、SNLS3和Planck + WMAP 9 + Wiggle Z $$ mathrm{Planck}+ WMAP9+mathrm{Wiggle}Z $$的观测数据集验证了重建的EoS参数符合文献中确定的约束条件。
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引用次数: 0
Reviewing the GR Method for Estimating Black Hole Parameters of Megamaser Systems 巨激光系统黑洞参数估计的GR方法综述
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-20 DOI: 10.1002/asna.20250016
Adriana González-Juárez, Alfredo Herrera-Aguilar

We review a general relativistic (GR) method to determine the black hole (BH) parameters: Mass-to-distance ratio, position, and recessional velocity of active galactic nuclei (AGNs) of Seyfert type, which have an accretion disk with water masers circulating around the BH. This GR method makes use of astrophysical observations: The redshifted and the blueshifted photons emitted from the aforementioned masers and their orbital position on the sky. In order to perform the estimations we implement a Bayesian statistical method to fit the above mentioned observational data. One of the main results of this work consists in analytically expressing the gravitational redshift, allowing us to quantify its magnitude for the photons emitted by the closest masers to the black holes. We present this quantity for several BHs hosted at the core of AGNs.

我们回顾了一种广义相对论(GR)方法来确定黑洞(BH)参数:Seyfert型活动星系核(agn)的质量距离比、位置和衰退速度,这些星系核在BH周围循环着一个带水脉泽的吸积盘。这种GR方法利用了天体物理观测:从上述脉泽发射的红移和蓝移光子及其在天空中的轨道位置。为了进行估计,我们采用贝叶斯统计方法对上述观测数据进行拟合。这项工作的主要成果之一是解析地表达了引力红移,使我们能够量化距离黑洞最近的脉泽发射的光子的大小。我们给出了在agn核心的几个黑洞的这个量。
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引用次数: 0
Redshift-Agnostic Machine Learning Classification: Unveiling Peak Performance in Galaxy, Star, and Quasar Classification (Using SDSS DR17) 红移不可知机器学习分类:揭示银河系、恒星和类星体分类中的峰值性能(使用SDSS DR17)
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-18 DOI: 10.1002/asna.20240057
Debashis Chatterjee, Prithwish Ghosh

Classification of galaxies, stars, and quasars using spectral data is fundamental to astronomy, but often relies heavily on redshift. This study evaluates the performance of 10 machine learning algorithms on SDSS data to classify these objects, with a particular focus on scenarios where redshift information is unavailable. Leveraging features such as “z,” “u,” “g,” “r,” “i,” and redshift, we assess the accuracy of various algorithms, including XGBoost, Random Forest, and recurrent neural networks (RNNs). Our analysis demonstrates the superior accuracy of the Random Forest classifier when redshift is included. The feature importance analysis reveals that “redshift” is the most critical feature, contributing 64.7% to the classification accuracy, followed by the “z” band (10.0%) and the “g” band (7.95%). However, even in the absence of redshift, XGBoost, Random Forest, and RNNs exhibit promising results, indicating the potential of photometric data for accurate classification. We systematically compare classification outcomes with and without redshift, revealing the relative importance of different features and identifying the most robust classifiers for redshift-limited scenarios. This research not only highlights the power of machine learning for astronomical classification but also provides a framework for reliable classification when redshift data is lacking. By uncovering the distinguishing spectral characteristics of galaxies, stars, and quasars that are independent of redshift, we open new avenues for efficient and accurate classification in large-scale photometric surveys and the study of faint, high-redshift objects.

利用光谱数据对星系、恒星和类星体进行分类是天文学的基础,但往往严重依赖于红移。本研究评估了10种机器学习算法在SDSS数据上的性能,以对这些对象进行分类,特别关注红移信息不可用的场景。利用“z”、“u”、“g”、“r”、“i”和红移等特征,我们评估了各种算法的准确性,包括XGBoost、随机森林和循环神经网络(rnn)。我们的分析表明,当考虑红移时,随机森林分类器的精度更高。特征重要性分析显示,“红移”是最关键的特征,对分类准确率的贡献率为64.7%,其次是“z”波段(10.0%)和“g”波段(7.95%)。然而,即使在没有红移的情况下,XGBoost、Random Forest和rnn也表现出了很好的结果,这表明了光度数据在准确分类方面的潜力。我们系统地比较了有红移和没有红移的分类结果,揭示了不同特征的相对重要性,并确定了红移受限场景下最鲁棒的分类器。这项研究不仅突出了机器学习在天文分类中的力量,而且在缺乏红移数据的情况下,为可靠的分类提供了一个框架。通过揭示独立于红移的星系、恒星和类星体的独特光谱特征,我们为大规模光度调查和研究微弱、高红移天体的有效和准确分类开辟了新的途径。
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引用次数: 0
Enhanced Kinematics and Distribution Characteristics of Upper Scorpius and Ophiuchus Associations Based on Gaia DR3 基于Gaia DR3的上天蝎座和蛇夫座组合运动学和分布特征增强
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-11 DOI: 10.1002/asna.20240082
W. H. Elsanhoury

The kinematics within the solar vicinity have revealed interesting features relevant to both stellar and Galactic structures. This study examines three stellar associations in the Upper Scorpius and Ophiuchus regions, along with their sub-samples among Gaia DR3. The calculated kinematics and velocity ellipsoid characteristics, including the mean spatial velocity components (U, V, and W; km s−1), yielding values of approximately (−5.84 ± 2.42, −16.14 ± 4.02, −7.31 ± 2.70; km s−1). USC and Oph associations velocity dispersion within the ellipsoid (σi,i=1,2,3$$ {sigma}_i,forall i=1,2,3 $$) was found to be (1.36 ± 0.02, 0.80 ± 0.01, 0.96 ± 0.01; km s−1), their mean solar motion (S$$ {S}_{odot } $$) was determined to be approximately 18.62 ± 4.32 km s−1, convergent point coordinates (Ao,Do$$ {A}_{mathrm{o}},{D}_{mathrm{o}} $$) were (95.91 ± 0.09°, −44.42 ± 0.02°), and Oort's constants, yielding A = 17.80 ± 0.24 km s−1 kpc−1 and B = −9.61 ± 0.32 km s−1 kpc−1. Finally, the density distribution function per absolute magnitudes of USC and Oph associations is examined to obtain both luminosity and mass functions; their analysis revealed the absence of any peaks or dips as consistent with other recent studies.

太阳附近的运动学揭示了与恒星和星系结构相关的有趣特征。本研究考察了上天蝎座和蛇夫座区域的三个恒星组合,以及它们在盖亚DR3中的亚样本。计算得到的运动学和速度椭球特征,包括平均空间速度分量(U、V和W);Km s−1),所得值约为(−5.84±2.42,−16.14±4.02,−7.31±2.70;km (s−1)。在椭球内(σ i,∀i = 1,2,3 $$ {sigma}_i,forall i=1,2,3 $$),发现USC和Oph关联的速度色散分别为(1.36±0.02,0.80±0.01,0.96±0.01;km s−1),它们的平均太阳运动(s⊙$$ {S}_{odot } $$)被确定为大约18.62±4.32 km s−1,收敛点坐标(A 0,D ($$ {A}_{mathrm{o}},{D}_{mathrm{o}} $$)分别为(95.91±0.09°,- 44.42±0.02°)和Oort常数,得到A = 17.80±0.24 km s−1 kpc−1和B = - 9.61±0.32 km s−1 kpc−1。最后,研究了USC和Oph星等的密度分布函数,得到了USC和Oph星等的光度和质量函数;他们的分析显示,与最近的其他研究一致,没有任何峰值或低谷。
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引用次数: 0
Analysis of a q-Deformed Covariant Algebra With the Fock-Tani Formalism 用Fock-Tani形式分析q-变形协变代数
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-09 DOI: 10.1002/asna.20250009
Ramiro R. B. de Souza, Dimiter Hadjimichef, César A. Zen Vasconcellos

Motivated by the difficulties in the quantization of spacetime, we study a q-deformed covariant algebra that imposes minimum position and momentum measurement uncertainties. We do this by invoking the Fock-Tani formalism, mainly used in atomic and nuclear physics. The results are promising for further calculation of physical predictions.

由于时空量子化的困难,我们研究了一种施加最小位置和动量测量不确定性的q变形协变代数。我们通过调用主要用于原子和核物理学的Fock-Tani形式主义来做到这一点。该结果为进一步计算物理预测提供了希望。
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引用次数: 0
Detection of Eclipses in the Cataclysmic Variable LAMOST J035913.61 + 405035.0 灾变变星LAMOST J035913.61 + 405035.0的日食探测
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-05 DOI: 10.1002/asna.20240124
V. P. Kozhevnikov

I conducted photometric observations of the cataclysmic variable LAMOST J035913.61 + 405035.0 and detected eclipses. During these observations, I recorded 14 eclipses over two groups of nights separated by 13 months. I accurately determined the orbital period of the system to be Porb=0.22834385±0.00000021$$ {P}_{mathrm{orb}}=0.228kern0.1em 343kern0.1em 85pm 0.000kern0.1em 000kern0.1em 21 $$ days. For the eclipses, I derived an ephemeris which is valid for a long time and suitable for studying changes in the orbital period. The out-of-eclipse magnitude of the star varied between 15.32 ± 0.02 and 17.25 ± 0.08 mag. As the brightness decreased, the eclipses became deeper and narrower. The average depth of eclipses was 1.35 ± 0.10 mag, and the average width at half-depth was 16.9 ± 0.7 min. I estimated the range of possible orbital inclinations to be between 72.8° and 76.0°, and the range of average absolute V-band magnitudes of the disc to be between 5.16 ± 0.15 and 5.44 ± 0.15 mag. Although based on the light curve from the ZTF survey, LAMOST J035913.61 + 405035.0 showed only small outbursts with amplitudes below 1.5 mag, it should be classified as a dwarf nova because the average disc brightness and mass transfer rate were below the limit of thermal instability.

我对变星LAMOST J035913.61 + 405035.0进行了光度观测,并探测到了日食。在这些观察中,我在两组相隔13个月的夜晚记录了14次日食。我准确地确定了该系统的轨道周期为P球= 0.228 343 85±0.000 000 21 $$ {P}_{mathrm{orb}}=0.228kern0.1em 343kern0.1em 85pm 0.000kern0.1em 000kern0.1em 21 $$天。对于日食,我推导出了一个长期有效的星历表,适合于研究轨道周期的变化。这颗恒星的月食外星等在15.32±0.02到17.25±0.08等之间,随着亮度的降低,月食变得更深、更窄。月食的平均深度为1.35±0.10等,半深度的平均宽度为16.9±0.7 min。我估计该星盘可能的轨道倾角范围在72.8°~ 76.0°之间,平均v波段绝对星等范围在5.16±0.15 ~ 5.44±0.15等之间。虽然根据ZTF调查的光度曲线,LAMOST J035913.61 + 405035.0只显示出幅度在1.5等以下的小爆发,但由于其平均星盘亮度和传质率都低于热不稳定性的极限,应该将其归类为矮新星。
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引用次数: 0
Holonomy Observables for the Turaev–Viro Model of Quantum Gravity 量子引力Turaev-Viro模型的完整观测
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-05 DOI: 10.1002/asna.20250010
V. M. G. Silveira, D. Hadjimichef, E. G. S. Luna, César A. Zen Vasconcellos

This paper presents a proposal for the study of holonomy observables for the Turaev–Viro model, a model of three-dimensional Loop Quantum Gravity with a positive cosmological constant. A review of central aspects of Loop Quantum Gravity and of a categorical formalism for discrete gauge theories is presented with the intent to contextualize the Turaev–Viro model within a more general setting, which clarifies the role of the Hopf algebra slq(2,)$$ {mathfrak{sl}}_qleft(2,mathrm{mathbb{C}}right) $$ in its construction. The key results on spin observables for the Turaev–Viro model and on holonomy observables for the Ponzano–Regge model are presented as an effort to develop a theory of holonomy observables for the Turaev–Viro model.

本文提出了具有正宇宙常数的三维环量子引力模型Turaev-Viro模型的完整观测值的研究建议。本文回顾了环量子引力和离散规范理论的绝对形式化的核心方面,旨在将Turaev-Viro模型放在更一般的环境中,从而澄清了Hopf代数sl q(2)的作用。在其结构中($$ {mathfrak{sl}}_qleft(2,mathrm{mathbb{C}}right) $$)。本文给出了Turaev-Viro模型的自旋观测值和Ponzano-Regge模型的完整观测值的关键结果,为建立Turaev-Viro模型的完整观测值理论做出了努力。
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引用次数: 0
Issue Information: Astron. Nachr. 1/2025 发行信息:Astron。乙酰。1/2025
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-02-02 DOI: 10.1002/asna.20259001
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引用次数: 0
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