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Spatial Extent of the Magnetic Influence of an Active Region on the Solar Atmosphere 活动区对太阳大气磁场影响的空间范围
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-17 DOI: 10.1002/asna.70040
Gottfried Mann, Frédéric Schuller

Solar activity can be witnessed in the form of sunspots and active regions, where the magnetic field is enhanced by up to a factor of 1000 as compared to that of the quiet Sun. In addition, solar activity manifests itself in terms of flares, jets, coronal mass ejections and the production of highly energetic particles. All these processes are governed by the solar magnetic field. Here we study the spatial reach of the influence of the magnetic field of active regions on the photosphere and in the solar corona. An active region is modelled by a magnetic dipole located under the photosphere. This simplified description allows us to study the spatial influence of an active region in the solar atmosphere in a rough but easy way. We find that the area of influence of the magnetic field of an active region on the solar atmosphere increases with both the maximum strength of the magnetic field in the active region and the depth of the dipole under the photosphere. For a typical active region, the magnetic field can be neglected for distances beyond ca. 700 Mm on the photosphere and two solar radii in the solar corona.

太阳活动可以以太阳黑子和活动区的形式被观察到,在这些活动区,磁场比安静的太阳增强了1000倍。此外,太阳活动还表现为耀斑、喷流、日冕物质抛射和高能粒子的产生。所有这些过程都受太阳磁场的支配。本文研究了活动区磁场对光球和日冕影响的空间范围。一个活跃区域是由位于光球下面的磁偶极子模拟的。这种简化的描述使我们能够以粗略但简单的方式研究太阳大气中活动区域的空间影响。我们发现,活动区的磁场对太阳大气的影响面积随着活动区的最大磁场强度和光球下的偶极子深度的增加而增加。对于一个典型的活动区域,在光球和日冕两个太阳半径以外的距离上,磁场可以忽略不计。
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引用次数: 0
Cosmic Inflation in an Extended Noncommutative Foliated Quantum Gravity: The Wave Function of the Universe 扩展非交换叶状量子引力中的宇宙暴胀:宇宙的波函数
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-16 DOI: 10.1002/asna.70039
Peter O. Hess, César A. Zen Vasconcellos, José de Freitas Pacheco, Fridolin Weber, Remo Ruffini, Dimiter Hadjimichef, Moisés Razeira, Benno Bodmann, Marcelo Netz-Marzola, Geovane Naysinger, Rodrigo Fraga da Silva, João G. G. Gimenez

We explore a noncommutative extension of branch-cut quantum gravity (BCQG), with a focus on its implications for early-universe inflation. Our framework builds on a three-field mini-superspace model involving a complex-valued cosmic-scale factor, a perfect-fluid field, and an inflaton-type scalar field. Using a Faddeev–Jackiw symplectic deformation of the conventional Poisson algebra, we construct a noncommutative phase space and derive a modified Wheeler–DeWitt equation. Analytic solutions to the wave function of the universe are obtained and analyzed. We show that noncommutativity induces coupling between ultraviolet and infrared modes, naturally leading to an inflationary phase without requiring fine-tuned initial conditions. This feature offers a novel alternative to standard inflationary models. We also discuss how the structure of the wave function in this framework may relate to primordial density perturbations. While some aspects of this theory remain speculative, the mathematical formulation provides a consistent path toward integrating quantum gravitational effects into early cosmological dynamics.

我们探索了分支切断量子引力(BCQG)的非交换扩展,重点研究了它对早期宇宙暴胀的影响。我们的框架建立在一个包含复值宇宙尺度因子、完美流体场和膨胀型标量场的三场迷你超空间模型之上。利用常规泊松代数的faddev - jackiw辛变形,构造了一个非交换相空间,并导出了一个修正的Wheeler-DeWitt方程。得到并分析了宇宙波函数的解析解。我们表明,非交换性诱导紫外和红外模式之间的耦合,自然导致暴胀阶段,而不需要微调初始条件。这一特征为标准暴胀模型提供了一种新颖的选择。我们还讨论了在这个框架中波函数的结构如何与原始密度摄动有关。虽然这个理论的某些方面仍然是推测性的,但数学公式为将量子引力效应整合到早期宇宙动力学中提供了一致的途径。
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引用次数: 0
Spectral Variations, Quiet Chromosphere and Flaring of Transition Region of AR Lac in UV and Gaia DR3 in the Field Open Cluster NGC 7209 ngc7209疏散星团中AR - Lac在UV和Gaia DR3中过渡区的光谱变化、安静色球和耀斑
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-14 DOI: 10.1002/asna.70037
Magdy R. Sanad, Yasser H. M. Hendy, Helal I. Abdel Rahman, Doaa Eid

We present Gaia DR3 data and estimated the cluster radius, color-magnitude diagram and the membership probability of the open cluster NGC 7209 using the machine learning algorithm pyUPMASK. We evaluated the membership probability of the RS CVn eclipsing binary system AR Lac. We reported International Ultraviolet Explorer (IUE) observations during the period (1979–1994) of the RS CVn eclipsing binary system AR Lac to describe the spectral behavior and the physical conditions in its atmosphere. The observations reveal indications of flare activity in the transition region. Besides the flaring activity, the emission lines show a range of variations between high, intermediate, and low flux values. The relation between line fluxes and orbital phases is found. The flaring activity is found in 1979, 1990, and 1994. The reddening of AR Lac was estimated from the 2200 Å absorption feature to be E(BV)=0$$ Eleft(B-Vright)=0 $$. The average mass loss rate is found to be 3.2×109Myear1$$ approx 3.2times {10}^{-9}{M}_{odot}kern0.1em {mathrm{year}}^{-1} $$, the average temperature of the emitting region is determined by using Planck's equation to be 9.2×104K$$ approx 9.2times {10}^4;mathrm{K} $$, the energy of

我们给出了Gaia DR3数据,并使用机器学习算法pyUPMASK估计了疏散星团NGC 7209的星团半径、色星等图和隶属概率。我们评估了RS CVn对双星系统AR Lac的隶属概率。本文报道了国际紫外探测器(IUE)在1979-1994年期间对RS CVn食双星系统AR Lac的观测,以描述其光谱行为和大气中的物理条件。观测结果揭示了过渡区耀斑活动的迹象。除了燃烧活动外,发射谱线还显示了高、中、低通量值之间的一系列变化。发现了线通量与轨道相位之间的关系。在1979年、1990年和1994年发现了燃烧活动。根据2200 Å吸收特征估计AR Lac的变红为E (B−V) = 0 $$ Eleft(B-Vright)=0 $$。平均质量损失率为≈3.2 × 10−9 M⊙年−1$$ approx 3.2times {10}^{-9}{M}_{odot}kern0.1em {mathrm{year}}^{-1} $$,发射区的平均温度由普朗克方程确定为≈9.2 × 10 4 K $$ approx 9.2times {10}^4;mathrm{K} $$,耀斑能量约为≈3.9 × 10 38 erg $$ approx 3.9times {10}^{38}mathrm{erg} $$。我们将光谱变化归因于底层磁场的循环行为,并将耀斑活动归因于三组分模型。
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引用次数: 0
General Relativistic Effects on Multipole Magnetic Field Evolution in Neutron Stars: Implications for High-Braking-Index Magnetars 中子星中多极磁场演化的广义相对论效应:对高制动指数磁星的启示
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-14 DOI: 10.1002/asna.70032
Zhifu Gao, Sheng-Nan Sun, Wen-Qi Ma, Hao Shan

Neutron stars, particularly magnetars, exhibit extreme physical conditions with some of the strongest magnetic fields in the universe. Understanding the evolution of these magnetic fields is crucial for interpreting their observed properties, such as high braking indices and X-ray emissions. In this work, we investigate the decay of multipole magnetic fields in neutron stars by incorporating general relativistic (GR) effects into the induction equations. We derive GR-corrected evolution equations for dipole (l=1$$ l=1 $$), quadrupole (l=2$$ l=2 $$), and octupole (l=3$$ l=3 $$) fields, considering both toroidal and poloidal components. Our calculations show that GR effects significantly extend the magnetic field decay timescales, with the redshift factor z0.23$$ zapprox 0.23 $$ for a typical neutron star. We find that the GR-corrected decay timescales better align with observed characteristics of magnetars. Additionally, we discuss the implications of our model for X-ray emissions and magnetic energy release rates in magnetars. Our results highlight the importance of GR corrections for accurate predictions of magnetic field evolution and related observational phenomena.

中子星,特别是磁星,表现出极端的物理条件,具有宇宙中最强的磁场。了解这些磁场的演变对于解释其观察到的特性至关重要,例如高制动指数和x射线发射。在这项工作中,我们通过将广义相对论(GR)效应纳入感应方程来研究中子星中多极磁场的衰减。我们推导了偶极子(l = 1 $$ l=1 $$)、四极子(l = 2 $$ l=2 $$)、和八极(l = 3 $$ l=3 $$)场,同时考虑环向和极向分量。我们的计算表明,GR效应显著地延长了磁场衰减时间尺度,典型中子星的红移因子z≈0.23 $$ zapprox 0.23 $$。我们发现gr校正后的衰变时间尺度与观测到的磁星特征更吻合。此外,我们还讨论了我们的模型对磁星中x射线发射和磁能释放率的影响。我们的研究结果强调了GR校正对于准确预测磁场演化和相关观测现象的重要性。
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引用次数: 0
High Resolution Radio Analysis of the Starburst Galaxy NGC 4527: Signatures of an AGN Core 星暴星系NGC 4527的高分辨率无线电分析:AGN核心的特征
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-14 DOI: 10.1002/asna.70036
C. A. Galante, G. E. Romero, J. Saponara, P. Benaglia

NGC 4527 is a nearby edge-on spiral galaxy with both starburst and AGN features, hosting a LINER nucleus. We present a radio study of the large-scale structure and nuclear region of this galaxy, based on new uGMRT observations at 700 and 1230 MHz. Our continuum maps reveal extended emission tracing the stellar disk, with no evidence of a radio halo. The spectral index distribution and the presence of PAHs across the disk are consistent with ongoing star formation. In the nuclear region we resolve three compact sources: one at the galactic centre and two symmetrically aligned with the major axis at 400$$ sim 400 $$ pc. The spectral index values and the destruction of PAHs in the central source, together with previously detected X-rays emission, suggest the presence of a low-luminosity AGN. The two off-centre sources are consistent with a star formation ring, coincident with a molecular gas ring previously reported. We explore a scenario where super-Eddington accretion onto the black hole drives a dense wind that falls back onto the disk, triggering star formation in a circumnuclear ring.

NGC 4527是一个边缘上的螺旋星系,同时具有星暴和AGN的特征,拥有一个LINER核。我们在700和1230 MHz的新uGMRT观测基础上,对这个星系的大尺度结构和核区进行了无线电研究。我们的连续图显示了延伸的辐射追踪恒星盘,没有射电晕的证据。光谱指数分布和多环芳烃的存在与正在进行的恒星形成一致。在核区,我们解析了三个致密源:一个在银河系中心,两个在~ 400 $$ sim 400 $$ pc处与长轴对称排列。光谱指数值和中心源中多环芳烃的破坏,以及先前检测到的x射线发射,表明存在低亮度AGN。这两个偏离中心的源与恒星形成环一致,与先前报道的分子气体环一致。我们探索了一种场景,即黑洞的超级爱丁顿吸积驱动稠密的风落回圆盘上,引发环核环中的恒星形成。
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引用次数: 0
Speckle Observations With PISCO in Calern (France): II. Astrometric Measurements of Visual Double Stars in 2017–2018 and New or Revised Orbits for A1913 AB, A1710, COU1394, BU1185, A122, A570, HU577, COU812, HU332, A2095 AB, and A884 法国Calern地区PISCO散斑观测[j]。2017-2018年双星观测及A1913 AB、A1710、COU1394、BU1185、A122、A570、HU577、COU812、HU332、A2095 AB和A884的新轨道或修正轨道
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-10 DOI: 10.1002/asna.70000
M. Scardia, J.-L. Prieur, J.-P. Rivet, D. Vernet, E. Aristidi, J. F. Ling, L. Piccotti, L. Pansecchi, R. W. Argyle, L. Abe, P. Bendjoya, L. Maccarini

We present relative astrometric measurements of visual double stars, made in 2017–2018 with the speckle camera PISCO at the 1-m Epsilon telescope of the C2PU facility (Observatoire de la Côte d'Azur, Calern site). Our observing list contains orbital couples as well as double stars whose motion is still uncertain. From our observations of 1400 multiple stars, we obtained 1376 new measurements with angular separations in the range 0.1$$ {0}^{{primeprime} }.1 $$8.5$$ {8}^{{primeprime} }.5 $$, and an average accuracy of 0.008$$ {0}^{{primeprime} }.008 $$. The mean error on the position angles is 0°.50. Most of the position angles were determined without the usual 180° ambiguity with the application of the direct vector auto-correlation technique and/or by inspection of the long integration files. We present new and revised orbits for A1913 AB, A1710, COU1394, BU1185, A122, A570, HU577, COU812, HU332, A2095 AB, and A884, partly derived from our PISCO observations. The corresponding estimated values for the masses of those systems are compatible with the spectral types.

我们展示了2017-2018年在C2PU设施(Observatoire de la Côte d'Azur, Calern站点)的1米Epsilon望远镜上使用PISCO散斑相机对视觉双星的相对天文测量结果。我们的观测列表包括轨道对以及运动仍不确定的双星。从我们对1400多颗恒星的观测中,我们获得了1376个新的测量值,角距在0″.1 $$ {0}^{{primeprime} }.1 $$ -范围内8″.5 $$ {8}^{{primeprime} }.5 $$,平均精度为0″.008 $$ {0}^{{primeprime} }.008 $$。位置角的平均误差为0°0.50。利用直接矢量自相关技术和/或通过检查长积分文件,大多数位置角度的确定没有通常的180°模糊。我们展示了A1913 AB、A1710、COU1394、BU1185、A122、A570、HU577、COU812、HU332、A2095 AB和A884的新轨道和修正轨道,部分来自于我们的PISCO观测。这些系统的质量估计值与光谱类型是一致的。
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引用次数: 0
Equation of State for Strongly Magnetized White Dwarfs 强磁化白矮星的状态方程
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-10 DOI: 10.1002/asna.70030
Gao-Wen Sun, Da-Lin He, Wan-Li Ma, De-Jun Zhu

Strongly magnetized white dwarfs, characterized by surface magnetic fields of 1091012$$ {10}^9-{10}^{12} $$ G, harbor extreme interior conditions that necessitate a reevaluation of the equation of state. Building upon Dong et al. (2023), this work advances the understanding of relativistic electron pressure in superhigh magnetic fields. We investigate the interplay between magnetic field strength and stellar properties, including density, mass-radius relations, and total pressure. Our results reveal that strong magnetization can significantly enhance white dwarf masses beyond the Chandrasekhar limit, with maximal magnetic fields reaching 1015$$ {10}^{15} $$ G. This study not only refines the theoretical framework for white dwarf magnetization but also provides a foundation for exploring magnetized neutron stars.

强磁化的白矮星,其表面磁场为10 9−10 12 $$ {10}^9-{10}^{12} $$ G,具有极端的内部条件,需要重新评估状态方程。在Dong等人(2023)的基础上,这项工作推进了对超高磁场中相对论性电子压力的理解。我们研究了磁场强度和恒星特性之间的相互作用,包括密度、质量-半径关系和总压力。我们的研究结果表明,强磁化可以显著增强白矮星质量,使其超过钱德拉塞卡极限,最大磁场达到10 15 $$ {10}^{15} $$ G.这一研究不仅完善了白矮星磁化的理论框架,而且为探索磁化中子星提供了基础。
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引用次数: 0
Stellar Evolution in Close Binaries: Processes and Outcomes 近距离双星的恒星演化:过程和结果
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-08 DOI: 10.1002/asna.70034
Omar Gustavo Benvenuto, María Alejandra De Vito, Leandro Bartolomeo Koninckx, Maite Echeveste, María Leonela Novarino, Jorge Ernesto Horvath

We discuss some aspects of stellar evolution in binary systems. While single stars can swell following the chemical evolution of their interior, stars belonging to binary systems cannot overflow the size of the Roche lobe, if so hydrostatic equilibrium is strictly impossible. The system is forced to exchange mass between its members through the inner Lagrangian point. In the first part of the paper, we discuss the standard evolution of binaries that have a non-degenerate donor star and a compact companion. We show that the model fails when to account for the occurrence of binary pulsars when they predict a long-standing mass transfer episode. Models including irradiation feedback and evaporation in close binaries are examined next. Following these sections, we discuss the case of systems with a black hole (BH). We show that if BHs are born non-rotating, binary interaction seems insufficient to speed them up, an indication that BH's rotation is a feature present at birth. Finally, we discuss Blue Straggler Stars detected in open and globular clusters. Since they cannot be understood as single-born stars, we evaluate one of the proposed channels is mass transfer in close binaries, and discuss its viability and the limitations of the present models.

我们讨论了双星系统中恒星演化的一些方面。虽然单星可以随着其内部的化学演化而膨胀,但属于双星系统的恒星不能超过罗氏叶的大小,如果是这样,流体静力平衡是严格不可能的。系统被迫通过内拉格朗日点在其成员之间交换质量。在本文的第一部分,我们讨论了具有非简并供星和紧伴星的双星的标准演化。我们表明,当模型预测长期的质量传递事件时,当考虑到双星脉冲星的发生时,模型失败了。研究了包括辐照反馈和近距离双星蒸发在内的模型。在这些部分之后,我们将讨论具有黑洞(BH)的系统。我们表明,如果黑洞一出生就不旋转,那么双星相互作用似乎不足以加速它们,这表明黑洞的旋转是一种出生时就存在的特征。最后,我们讨论了在疏散星团和球状星团中发现的蓝离散星。由于它们不能被理解为单星,我们评估了其中一个被提出的通道是近双星的质量传递,并讨论了它的可行性和现有模型的局限性。
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引用次数: 0
The Gaia RVS Benchmark Stars. III. Confirmed and New High Radial Velocity Stars From Gaia DR3 盖亚RVS基准星。3。来自盖亚DR3的确认和新的高径向速度恒星
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-07 DOI: 10.1002/asna.70025
Elisabetta Caffau, David Katz, Piercarlo Bonifacio, Ana Gómez, Rosine Lallement, Paola Sartoretti, Frédéric Royer, Pasquale Panuzzo, Monique Spite, Patrick François, Nicolas Leclerc, Luca Sbordone, Frédéric Thévenin, Hans-Günter Ludwig, Laurent Chemin

High-velocity stars are interesting targets to unveil the formation of the Milky Way. In fact they can be recently accreted from an infalling dwarf galaxies or they can be the result of a turbulent merging of galaxies. Gaia is providing the community a way to select stars for their kinematics and the radial velocity, one of the speed components, is derived from the Gaia RVS spectrum. High absolute radial velocity values are sensitive to be false positive. They are rare and as such they are more easily impacted than lower velocity stars, by contamination by very low SNR spurious measures. We here investigate a sample of 26 stars with Gaia absolute radial velocity in excess of 500 km/s with spectroscopic follow-up observations with UVES. For all but one star the extreme radial velocity is confirmed and these stars are all metal-poor and, as expected, enhanced in the α$$ alpha $$ elements. The complete chemical inventory confirm the large star-to-star scatter for the heavy elements and their on average larger ratio over iron with respect to the Sun, in agreement with the literature.

高速恒星是揭示银河系形成的有趣目标。事实上,它们可能是最近从坠落的矮星系中吸积起来的,也可能是星系湍流合并的结果。盖亚为社区提供了一种选择恒星运动学和径向速度的方法,径向速度是速度分量之一,来自盖亚RVS光谱。较高的绝对径向速度值容易出现假阳性。它们是罕见的,因此它们比速度较低的恒星更容易受到影响,被非常低信噪比的伪测量污染。本文对26颗盖亚绝对视向速度超过500 km/s的恒星样本进行了UVES光谱跟踪观测。除了一颗恒星外,所有恒星都证实了极端径向速度,这些恒星都是金属贫乏的,正如预期的那样,α $$ alpha $$元素增加了。完整的化学清单证实了重元素在恒星间的大散射,以及它们相对于太阳的平均比大于铁的比例,这与文献一致。
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引用次数: 0
Cosmological Confusion: A Brief Appraisal 宇宙学的困惑:一个简短的评价
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-07-07 DOI: 10.1002/asna.70033
J. E. Horvath

We examine in this brief review some of the emerging controversies and problems of the standard Λ$$ Lambda $$CDM Cosmology. We make a few autobiographical notes and point out two psychological/sociological attitudes that may difficult the solution of the problems and therefore to the advance on the discipline. Criticisms to Inflation and Large-Scale Structure are exposed, and the general construction of a consensual Cosmology, even a non-standard one, highlighted.

在这篇简短的综述中,我们研究了一些关于标准Λ $$ Lambda $$ CDM宇宙学的新出现的争议和问题。我们做了一些自传式的笔记,并指出了两种心理学/社会学的态度,这可能会阻碍问题的解决,从而阻碍学科的发展。对暴胀论和大尺度结构论的批评被揭露,共识宇宙论的一般建构,甚至是非标准宇宙论的建构都被强调。
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引用次数: 0
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Astronomische Nachrichten
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