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Issue Information: Astron. Nachr. 5/2025 发行信息:Astron。乙酰。5/2025
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-25 DOI: 10.1002/asna.70026
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引用次数: 0
Multiwavelength Activity of NGC 1275 Nucleus NGC 1275核的多波长活动
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-18 DOI: 10.1002/asna.70023
Vera G. Sinitsyna, Vera Y. Sinitsyna, S. S. Borisov

Active galactic nucleus (AGN) phenomenon and role of jets, powered by the central black hole of AGN, in the feedback of the surroundings on different scales is a matter of detailed multi-wavelength investigations. The long-term observations of AGN are used to reveal the processes taking place in the very proximity to the super-massive black holes. One of the approaches to such studies is to detect the launching of jet components viewed in the radio range and then link it with flaring events detected at higher energy ranges. Tracking the jet-initiated variability events through multiwavelength observations as well as their cross-identification from radio frequencies up to high-energy gamma-rays allows one to locate the regions responsible for the generation of observable features, which can lead to the exploration of the mechanism of jet launching and the origin of emission in the Active Galactic Nucleus. Being nearby and bright, NGC 1275 is one of the extensively studied AGN. This object is very active in the timescales of decades. Multiwavelength long-term observations of NGC 1275 resulted in the detection of different timescale variability from this AGN. For the case of NGC 1275, the cross-correlation of the activity at radio, X-ray, and very high-energy gamma-rays is investigated. The time dependence of the activity of NGC 1275 in the wide energy range was found, which allows one to localize the sites of the emission generation, including one of the very high energies. These multiwavelength long-term studies are highly important for the further advance of the AGN's black hole research and investigations of mechanisms of jet formation.

活动星系核(AGN)的中心黑洞提供能量的喷流现象及其在不同尺度上对周围环境的反馈作用是一个详细的多波长研究问题。AGN的长期观测被用来揭示发生在超大质量黑洞附近的过程。这类研究的方法之一是探测在无线电范围内观测到的喷射成分的发射,然后将其与在更高能量范围内探测到的燃烧事件联系起来。通过多波长观测以及从无线电频率到高能伽马射线的交叉识别来跟踪喷流引发的变异性事件,可以确定产生可观测特征的区域,从而可以探索喷流发射的机制和活动星系核中发射的起源。NGC 1275离我们很近,而且明亮,是被广泛研究的AGN之一。这个天体在几十年的时间尺度上非常活跃。通过对NGC 1275的多波长长期观测,发现了该AGN的不同时间尺度变化。以NGC 1275为例,研究了射电、x射线和高能伽马射线活动的相互关系。发现了NGC 1275在较宽能量范围内活动的时间依赖性,这使得人们可以定位辐射产生的位置,包括一个非常高的能量。这些多波长的长期研究对于进一步推进AGN黑洞研究和射流形成机制的研究具有重要意义。
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引用次数: 0
Mkn 180 BL Lac Type Object Viewed at High and Very-High Energies mkn180bl Lac型天体在高能量和甚高能量下的观测
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-17 DOI: 10.1002/asna.70022
Vera G. Sinitsyna, Vera Y. Sinitsyna

Blazars are among the most powerful objects in the Universe, whose photon spectrum extends from radio to very high energy gamma-rays (γ-rays). Spectral energy distribution (SED) of blazars has a two-humped shape, whose low-energy part originates from the leptonic mechanism of synchrotron radiation of relativistic electrons in the blazars' jets. It is generally believed that the high-energy part of the spectral energy distribution is of hadronic and leptonic scenarios, but different localization of the source of emission within the core region or far beyond is considered. Also, blazars' emission is characterized by rapid variability at all wavelengths. The tracking of the flaring events at the radio band to connected ones at higher energies may allow localizing emission regions. High-frequency peaked Bl Lacertae type of blazar objects (HBL) are characterized by multi-wavelength variability and SED peaking at the GeV–TeV energy range. Thus, HBL objects have been considered as the best candidate for the sources of very high γ-rays. Mkn 180 is the HBL object with the spectrum that has been measured through radio and X-ray bands to high energy γ-rays. The study of the connection between the outbursts from Mkn 180 viewed from radio to very high energy γ-rays is presented together with its features at the MeV–TeV energy range. These results can help find the parameters for the models of generation of high-energy γ-ray emission in Bl Lac-type objects.

耀变体是宇宙中最强大的物体之一,其光子光谱从无线电延伸到非常高能的伽马射线(γ射线)。耀变体的光谱能量分布呈双峰状,其低能部分源于耀变体喷流中相对论性电子同步辐射的轻子机制。一般认为光谱能量分布的高能部分是强子和轻子两种情况,但也考虑了辐射源在核心区内或远远超出核心区的不同定位。此外,耀变体的发射在所有波长上都具有快速变化的特征。将无线电波段上的燃烧事件跟踪到更高能量的连接事件,可以确定发射区域的局部化。brertae型blazar天体(HBL)的高频峰具有多波长变异性和GeV-TeV能量范围内的SED峰。因此,HBL天体被认为是非常高γ射线的最佳候选源。Mkn 180是HBL天体,其光谱已经通过无线电和x射线波段测量到高能γ射线。本文介绍了mkn180从射电观测到的爆发与高能γ射线之间的联系及其在MeV-TeV能量范围内的特征。这些结果有助于寻找Bl - lac型天体高能γ射线产生模型的参数。
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引用次数: 0
Mechanisms of High Energy Emission From Mkn 180 BL Lacertae Object mkn180bl星带天体高能发射的机制
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-16 DOI: 10.1002/asna.70018
Vera G. Sinitsyna, Vera Y. Sinitsyna

Mkn 180 is the BL Lac object with the spectrum that has been measured through radio and x-ray band to high energy gamma-rays. This object is considered as a potential candidate for the source of high-energy leptonic and/or hadronic cosmic-ray acceleration. Also, it has been proposed to be a GeV–TeV gamma-ray source. The very high energy gamma-rays from Mkn 180 were detected due to the trigger switched on by an optical burst. Mkn 180 was monitored in the optical wave band and in the high and very high energy gamma-rays for a long period and its light curve was obtained. The spectral energy distribution of Mkn 180 blazar was obtained in the wide energy range as well. The spectral energy distributions of blazars consist of two broad peaks. The first, lower frequency peak occurring between radio and soft x-ray energies is due to the synchrotron emissions of relativistic electrons population. Leptonic and hadronic emission mechanisms are considered to describe the second, higher frequency spectrum part between x-ray and VHE gamma-ray energies. The Inverse Compton emissions of the same electrons (synchrotron self-Compton model) or combined with an external Compton mechanism originating from the broad-line region, or the accretion disk are considered in the leptonic scenario. Also, the high energy spectrum part is supposed to be generated due to the processes of photohadronic or hadronuclear interactions of cosmic rays with radiation or matter in the AGN's jet emission region. The multiwavelength observations of Mkn 180 including the GeV–TeV energy data can help to clarify the dominant mechanism of generation of high-energy gamma-ray emission in this object (and whether it can be the source of UHECRs).

Mkn 180是BL Lac天体,其光谱已经通过无线电和x射线波段到高能伽马射线进行了测量。该天体被认为是高能轻子和/或强子宇宙射线加速源的潜在候选者。此外,它也被认为是GeV-TeV的伽马射线源。来自mkn180的高能伽马射线被探测到,这是由于一个光学爆发打开了触发器。在光波波段和高能、甚高能伽马射线波段对mkn180进行了长时间的监测,得到了它的出光曲线。得到了mkn180在较宽能量范围内的光谱能量分布。耀变体的光谱能量分布由两个宽峰组成。第一个频率较低的峰值发生在无线电和软x射线能量之间,是由于相对论电子种群的同步辐射。轻子和强子发射机制被认为描述了x射线和VHE伽玛射线能量之间的第二个更高频谱部分。在轻子情景中考虑了相同电子的逆康普顿发射(同步自康普顿模型)或与来自宽线区域或吸积盘的外部康普顿机制相结合。此外,高能谱部分应该是由于宇宙射线与AGN喷流发射区的辐射或物质的光强子或强核相互作用过程而产生的。Mkn 180的多波长观测,包括GeV-TeV能量数据,可以帮助阐明该天体产生高能伽马射线的主要机制(以及它是否可能是uhecr的来源)。
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引用次数: 0
Uncertainties in Ground-Based Visual Double Star Measures—II Accuracy of Measures 地面视觉双星测量中的不确定性——ii测量精度
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-16 DOI: 10.1002/asna.70015
Graeme L. White, Roderick R. Letchford

Letchford and White 2025, Paper I, determined the uncertainties in ground-based historic measures of double stars. In this paper, the accuracy of 26,205 ground-based measures of 857 visual double stars, made since $$ sim $$1780, is determined relative to space-based measures based on positions and proper motion from the HIPPARCOS (via ASCC) and Gaia DR3 missions. We determine the accuracy of measures for the epoch of observation, the size of the telescope, the different attached instruments, and the filter applied. We find that the accuracy of the measures is improving with time; however, the typical telescope used for double-star observations has been, and continues to be, relatively small. Modern instrumentation such as speckle interferometry and lucky imaging has advanced the accuracy by a factor of ten over traditional micrometre measurements.

Letchford和White 2025,论文1,确定了基于地面的双星历史测量的不确定性。在本文中,相对于HIPPARCOS(通过ASCC)和Gaia DR3任务基于位置和适当运动的天基测量,确定了自$$ sim $$ 1780年以来对857颗视觉双星进行的26,205次地面测量的精度。我们确定了观测历元、望远镜的大小、不同的附加仪器和应用的滤光片的测量精度。我们发现测量的准确性随着时间的推移而提高;然而,用于双星观测的典型望远镜一直是,而且将继续是相对较小的。像散斑干涉测量和幸运成像这样的现代仪器比传统的微米测量精度提高了十倍。
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引用次数: 0
Impact of Topological Structures on Neutron Star Rotation and Their Observational Significance 拓扑结构对中子星旋转的影响及其观测意义
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-15 DOI: 10.1002/asna.70017
Debojoti Kuzur

Rotational irregularities are one of the prominent observational features that most pulsars exhibit. These glitches, which are sudden increases in spin angular velocity, remains an open problem. In this study, we have investigated the potential role of nontrivial topological defects, specifically in the form of Nambu-Goto type cosmic strings, and its connection to spin irregularities. Such cosmic strings which are one-dimensional topological defects may be formed during various symmetry-breaking and phase transition scenarios and can interact with the neutron stars. In this work, we see that the appearance of such topological defects trapped within the core can lead to the coupling of the string tension with the angular velocity, leading to the abrupt rotational changes observed as pulsar glitches. Further we see, these coupling may generate detectable gravitational waves as a mixture of continuous and burst signals. The evolution of cusps of cosmic strings trapped within neutron stars and the neutron star's mass quadruple moment change due to rotation could produce distinctive gravitational wave signatures, well within the noise cutoff of advLIGO. Our study highlights a potential connection between topological defects, pulsar glitches, and gravitational wave emissions, offering a possible avenue for observationally testing their astrophysical effects.

旋转不规则是大多数脉冲星表现出的显著观测特征之一。这些小故障,即旋转角速度的突然增加,仍然是一个悬而未决的问题。在这项研究中,我们研究了非平凡拓扑缺陷的潜在作用,特别是以Nambu-Goto型宇宙弦的形式,以及它与自旋不规则性的联系。这种宇宙弦是一种一维拓扑缺陷,可以在各种对称破缺和相变情况下形成,并能与中子星相互作用。在这项工作中,我们看到这种被困在核心内的拓扑缺陷的出现会导致弦张力与角速度的耦合,导致在脉冲星故障时观察到的突然旋转变化。我们进一步看到,这些耦合可能会产生可探测的引力波,作为连续和突发信号的混合物。中子星内部宇宙弦尖的演化和中子星因旋转而产生的质量四倍矩变化可以产生独特的引力波特征,完全在advLIGO的噪声截止范围内。我们的研究强调了拓扑缺陷、脉冲星故障和引力波发射之间的潜在联系,为观测测试它们的天体物理效应提供了可能的途径。
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引用次数: 0
Study of the Structure of Interstellar Medium Towards the Star 62 Tau With ESPRESSO Spectrograph 用ESPRESSO光谱仪研究62 Tau星的星际介质结构
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-15 DOI: 10.1002/asna.70016
Arkadii Bondar, Jacek Krełowski

We have conducted investigations of the structure of interstellar medium towards the star 62 Tau using a very high resolving power (R = λ/δλ$$ lambda /delta lambda sim $$170 000) spectrum of ESPRESSO spectrograph. Basic goals of this work are as follows: to search for radial velocity components in the interstellar spectral lines, detectable in the star's spectrum; to measure heliocentric radial velocities (Vr) of the intervening interstellar clouds, to determine Doppler parameter b and the column densities (N) of the atoms and molecules present in the clouds. Using a profile fit procedure we found the components of the atomic and molecular lines with the Vr between $$ approx $$11–18.5 km s1$$ {}^{-1} $$. Only two main radial velocity components for every spectral feature could be discerned confidently. Thus, it was found that the interstellar matter on this sightline is mostly concentrated in the interstellar clouds with Vr$$ approx $$ 15 and 18 km s1$$ {}^{-1} $$. The column densities, yielded with the profile fits are in a good agreement with those found earlier by other researchers. The profiles of the interstellar molecular lines (CN, CH and CH

我们利用高分辨率(R = λ / δ λ ~ $$ lambda /delta lambda sim $$ 170000)的ESPRESSO光谱仪对62 Tau恒星的星际介质结构进行了研究。这项工作的基本目标是:在恒星光谱中可探测到的星际光谱线中寻找径向速度分量;测量中间星际云的日心径向速度(Vr),确定多普勒参数b和存在于云中的原子和分子的柱密度(N)。利用剖面拟合程序,我们发现了Vr在≈$$ approx $$ 11-18.5 km s−1 $$ {}^{-1} $$之间的原子和分子线的组成部分。每个光谱特征只有两个主要的径向速度分量可以确定。因此,在这条视线上的星际物质主要集中在Vr≈$$ approx $$ 15和18 km s−1的星际云中$$ {}^{-1} $$。用剖面拟合得到的柱密度与其他研究人员早先发现的密度很一致。首次以如此高的分辨率分析了该恒星光谱中的星际分子谱线(CN, CH和CH + $$ {}^{+} $$)。
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引用次数: 0
Very High Energy Observations of Low-Mass X-Ray Binary 4U 2129+47 低质量x射线双星4U 2129+47的高能观测
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-15 DOI: 10.1002/asna.70019
Vera G. Sinitsyna, Vera Y. Sinitsyna

4U 2129+47 is classified as a low-mass x-ray binary containing a neutron star. It is actively studied in the optical and x-ray. It was found that this binary exhibits both the outburst and quiescent states. The spectroscopic investigations of the optical counterpart of the neutron star in this binary system showed that the 4U 2129+47 is a hierarchical triple system. X-ray observations showed the evidence for a spatially extended Accretion Disk Corona. This type of objects is considered as a possible source of high energy emission generated due to the interaction between the wind of the neutron star pulsar and accretion disk. Observations of 4U 2129+47 system with SHALON telescope were performed in the period 1999–2011 years. Weak gamma-ray emission from this object was detected with the significance of 11.6σ. An integral flux above > 0.8 GeV was measured. The modulation of detected gamma-ray emission with the orbital period of 5.24 h is found. The hard differential spectrum with the photon index of −1.49 ± 0.13 has been determined. Detected modulation of TeV gamma-ray flux with orbit together with the hard tail of soft x-rays detected with Chandra can be evidence of active accretion and also may point to the generation of emission through the interaction of the wind and accretion stream.

4U 2129+47被归类为含有中子星的低质量x射线双星。它在光学和x射线中得到了积极的研究。发现该双星同时具有爆发态和静止态。对该双星系统中子星光学对应体的光谱研究表明,4U 2129+47是一个分层三重系统。x射线观测显示了空间扩展的吸积盘日冕的证据。这种类型的天体被认为是由于中子星脉冲星风和吸积盘之间的相互作用而产生的高能发射的可能来源。利用SHALON望远镜对4U 2129+47系统进行了1999-2011年的观测。探测到该天体微弱的伽马射线发射,显著性为11.6σ。测量到的积分通量大于0.8 GeV。发现了轨道周期为5.24 h的伽马射线发射调制。测定了光子指数为- 1.49±0.13的硬微分光谱。探测到的TeV伽玛射线通量与轨道的调制以及钱德拉探测到的软x射线的硬尾可以作为活跃吸积的证据,也可能指出通过风和吸积流的相互作用产生发射。
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引用次数: 0
XMM-Newton Publications From 2000 to 2024 从2000年到2024年
IF 1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-12 DOI: 10.1002/asna.70014
Jan-Uwe Ness, Norbert Schartel, Maria Santos-Lleo
<div> <p><i>XMM-Newton</i> is an ESA space x-ray observatory launched on 11 December 1999, and after 25 years, a study is presented demonstrating that the data of the mission are efficiently used by an engaged and productive community. The total number of refereed papers published between 2000 and 2024 is 8486. These papers have a total of 15,627 different authors, including 3292 unique first authors. The total available science time during this period amounts to 556 Ms (16,894 observations) 87% of which (84% of observations) have been used in at least one refereed publication, excluding primary catalogue papers. Accounting for multiple use, the observation time has been over-used by a factor of up to 15 in dedicated publications and even a factor of up to 30 when including a small fraction of papers classified as survey/catalogue. The speed with which observations are published for the first time peaks around 2 years and is thus longer than the proprietary period for Guest–Observer (GO) observations. A strong secondary peak at 3 years suggests that data not published by the proposing teams are picked up by the community, then also taking about 2 years to be published. The publication rate remains stable at <span></span><math> <semantics> <mrow> <mo>∼</mo> <mn>400</mn> </mrow> <annotation>$$ sim 400 $$</annotation> </semantics></math> refereed articles per year with a small increase in recent years, owed to an increased use of primary <i>XMM-Newton</i> catalogues. 95% of articles focus on specific data using <span></span><math> <semantics> <mrow> <mo><</mo> <mn>49</mn> </mrow> <annotation>$$ <49 $$</annotation> </semantics></math> observations while 99% of articles use less than 239 observations. Since 2010, the annual number of first-time authors has remained relatively constant, equalling the number of last-time authors. This implies that the number of scientists engaged in research utilising <i>XMM-Newton</i> data has remained constant at 4300, of whom 570 are lead (first) authors. A histogram of the activity period demonstrates that 51% of first authors publish for only 1 year, 24% of first authors are active for up to 6 years, and 25% were active for more than 6 years. We further identify a highly productive core community of approximately 120 scientists publishing an <i>XMM-Newton</i> article at least every 2 year as first authors. When all authors are considered, the figures are 40%, 25% and 35%, respectively. The considerable number of time-limited activities may reflect a high level of utilisation during the early stages of a research career, from Master's studies through the PhD and initial postdoctoral years. The trends assessed indicate a vital community with positive perspectives and a continued, active
xmm -牛顿是欧空局于1999年12月11日发射的空间x射线天文台,经过25年的发展,一项研究表明,该任务的数据被一个积极参与和富有成效的社区有效地利用。2000年至2024年间发表的评审论文总数为8486篇。这些论文共有15627位不同的作者,其中包括3292位独特的第一作者。在此期间,总可用科学时间达556毫秒(16,894次观测)87% of which (84% of observations) have been used in at least one refereed publication, excluding primary catalogue papers. Accounting for multiple use, the observation time has been over-used by a factor of up to 15 in dedicated publications and even a factor of up to 30 when including a small fraction of papers classified as survey/catalogue. The speed with which observations are published for the first time peaks around 2 years and is thus longer than the proprietary period for Guest–Observer (GO) observations. A strong secondary peak at 3 years suggests that data not published by the proposing teams are picked up by the community, then also taking about 2 years to be published. The publication rate remains stable at ∼ 400 $$ sim 400 $$ refereed articles per year with a small increase in recent years, owed to an increased use of primary XMM-Newton catalogues. 95% of articles focus on specific data using < 49 $$ <49 $$ observations while 99% of articles use less than 239 observations. Since 2010, the annual number of first-time authors has remained relatively constant, equalling the number of last-time authors. This implies that the number of scientists engaged in research utilising XMM-Newton data has remained constant at 4300, of whom 570 are lead (first) authors. A histogram of the activity period demonstrates that 51% of first authors publish for only 1 year, 24% of first authors are active for up to 6 years, and 25% were active for more than 6 years. We further identify a highly productive core community of approximately 120 scientists publishing an XMM-Newton article at least every 2 year as first authors. When all authors are considered, the figures are 40%, 25% and 35%, respectively. The considerable number of time-limited activities may reflect a high level of utilisation during the early stages of a research career, from Master's studies through the PhD and initial postdoctoral years. The trends assessed indicate a vital community with positive perspectives and a continued, active interest in XMM-Newton for the future.
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引用次数: 0
Cover Picture: Astron. Nachr. 3/2025 封面图片:Astron。乙酰。3/2025
IF 1.1 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS Pub Date : 2025-06-03 DOI: 10.1002/asna.70013
J. E. Horvath

The wide variety of topics discussed at the IWARA 2014 workshop in Machu Picchu, Peru, and their relation to a large range of disciplines from archaeology to cosmology is illustrated schematically in this artwork. Names point out authors among the IWARA participants who wrote scientific contributions in the respective field of research. The chart may be taken as a guide to explore the publications in this Special Issue of AN. Some interesting philosophical comments about the science discussed (and not discussed) at the workshop can be found in the Concluding Remarks by J.E. Horvath (e240137).

在秘鲁马丘比丘举行的IWARA 2014研讨会上讨论的各种主题,以及它们与从考古学到宇宙学的广泛学科的关系,在这幅艺术作品中得到了简要的说明。名字指的是IWARA参与者中在各自研究领域撰写科学贡献的作者。此图表可作为浏览《亚洲新闻报》特刊刊物的指引。在J.E. Horvath的结束语(e240137)中可以找到一些关于研讨会上讨论(或未讨论)的科学的有趣的哲学评论。
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引用次数: 0
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Astronomische Nachrichten
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