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Global seismology of the Sun 全球太阳地震学
IF 20.9 1区 物理与天体物理 Pub Date : 2016-08-08 DOI: 10.1007/s41116-016-0003-4
Sarbani Basu

The seismic study of the Sun and other stars offers a unique window into the interior of these stars. Thanks to helioseismology, we know the structure of the Sun to admirable precision. In fact, our knowledge is good enough to use the Sun as a laboratory. We have also been able to study the dynamics of the Sun in great detail. Helioseismic data also allow us to probe the changes that take place in the Sun as solar activity waxes and wanes. The seismic study of stars other than the Sun is a fairly new endeavour, but we are making great strides in this field. In this review I discuss some of the techniques used in helioseismic analyses and the results obtained using those techniques. I focus on results obtained with global helioseismology, i.e., the study of the Sun using its normal modes of oscillation. I also briefly touch upon asteroseismology, the seismic study of stars other than the Sun, and discuss how seismic data of others stars are interpreted.

对太阳和其他恒星的地震研究为了解这些恒星的内部提供了一个独特的窗口。由于日震学,我们对太阳结构的了解精确到令人钦佩的程度。事实上,我们的知识足以把太阳当作一个实验室。我们还能够非常详细地研究太阳的动力学。日震数据还使我们能够探测到太阳活动时发生的变化。对太阳以外的恒星进行地震研究是一项相当新的努力,但我们在这一领域取得了很大的进展。在这篇综述中,我讨论了一些用于日震分析的技术和使用这些技术所获得的结果。我着重于用全球日震学获得的结果,即利用太阳的正常振荡模式来研究太阳。我还简要介绍了星震学,即对太阳以外的恒星进行地震研究,并讨论了如何解释其他恒星的地震数据。
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引用次数: 79
Solar and stellar photospheric abundances 太阳和恒星的光球丰度
IF 20.9 1区 物理与天体物理 Pub Date : 2016-07-05 DOI: 10.1007/s41116-016-0001-6
Carlos Allende Prieto

The determination of photospheric abundances in late-type stars from spectroscopic observations is a well-established field, built on solid theoretical foundations. Improving those foundations to refine the accuracy of the inferred abundances has proven challenging, but progress has been made. In parallel, developments on instrumentation, chiefly regarding multi-object spectroscopy, have been spectacular, and a number of projects are collecting large numbers of observations for stars across the Milky Way and nearby galaxies, promising important advances in our understanding of galaxy formation and evolution. After providing a brief description of the basic physics and input data involved in the analysis of stellar spectra, a review is made of the analysis steps, and the available tools to cope with large observational efforts. The paper closes with a quick overview of relevant ongoing and planned spectroscopic surveys, and highlights of recent research on photospheric abundances.

通过光谱观测确定晚型恒星的光球丰度是一个建立在坚实理论基础上的成熟领域。事实证明,改进这些基础以提高推断丰度的准确性具有挑战性,但已经取得了进展。与此同时,仪器的发展,主要是关于多目标光谱学,已经取得了惊人的进展,许多项目正在收集银河系和附近星系的大量恒星观测数据,有望在我们对星系形成和演化的理解方面取得重要进展。在简要介绍了恒星光谱分析的基本物理和输入数据后,回顾了分析步骤,以及处理大型观测工作的可用工具。本文最后简要概述了相关的正在进行的和计划中的光谱调查,并强调了最近对光球丰度的研究。
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引用次数: 15
Oscillations and Waves in Sunspots 太阳黑子的振荡和波动
IF 20.9 1区 物理与天体物理 Pub Date : 2015-12-01 DOI: 10.1007/lrsp-2015-6
Elena Khomenko, Manuel Collados

A magnetic field modifies the properties of waves in a complex way. Significant advances have been made recently in our understanding of the physics of sunspot waves with the help of high-resolution observations, analytical theories, as well as numerical simulations. We review the current ideas in the field, providing the most coherent picture of sunspot oscillations as by present understanding.

磁场以一种复杂的方式改变波的性质。最近,在高分辨率观测、分析理论和数值模拟的帮助下,我们对太阳黑子波物理学的理解取得了重大进展。我们回顾了该领域目前的观点,提供了目前了解的太阳黑子振荡的最连贯的画面。
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引用次数: 111
Interaction Between Convection and Pulsation 对流和脉动之间的相互作用
IF 20.9 1区 物理与天体物理 Pub Date : 2015-12-01 DOI: 10.1007/lrsp-2015-8
Günter Houdek, Marc-Antoine Dupret

This article reviews our current understanding of modelling convection dynamics in stars. Several semi-analytical time-dependent convection models have been proposed for pulsating one-dimensional stellar structures with different formulations for how the convective turbulent velocity field couples with the global stellar oscillations. In this review we put emphasis on two, widely used, time-dependent convection formulations for estimating pulsation properties in one-dimensional stellar models. Applications to pulsating stars are presented with results for oscillation properties, such as the effects of convection dynamics on the oscillation frequencies, or the stability of pulsation modes, in classical pulsators and in stars supporting solar-type oscillations.

本文综述了我们目前对恒星对流动力学建模的理解。对于脉动的一维恒星结构,提出了几种半解析的时变对流模型,它们具有不同的对流湍流速度场如何与恒星整体振荡耦合的公式。在这篇综述中,我们把重点放在两个,广泛使用的,时变对流公式估计脉动特性在一维恒星模型。应用于脉动恒星,给出了振荡特性的结果,如对流动力学对振荡频率的影响,或脉动模式的稳定性,在经典脉动星和支持太阳型振荡的恒星。
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引用次数: 43
The Solar Cycle 太阳周期
IF 20.9 1区 物理与天体物理 Pub Date : 2015-09-21 DOI: 10.1007/lrsp-2015-4
David H. Hathaway

The solar cycle is reviewed. The 11-year cycle of solar activity is characterized by the rise and fall in the numbers and surface area of sunspots. A number of other solar activity indicators also vary in association with the sunspots including; the 10.7 cm radio flux, the total solar irradiance, the magnetic field, flares and coronal mass ejections, geomagnetic activity, galactic cosmic ray fluxes, and radioisotopes in tree rings and ice cores. Individual solar cycles are characterized by their maxima and minima, cycle periods and amplitudes, cycle shape, the equatorward drift of the active latitudes, hemispheric asymmetries, and active longitudes. Cycle-to-cycle variability includes the Maunder Minimum, the Gleissberg Cycle, and the Gnevyshev-Ohl (even-odd) Rule. Short-term variability includes the 154-day periodicity, quasi-biennial variations, and double-peaked maxima. We conclude with an examination of prediction techniques for the solar cycle and a closer look at cycles 23 and 24.

回顾了太阳周期。太阳活动的11年周期的特点是太阳黑子的数量和表面积的上升和下降。其他一些太阳活动指标也与太阳黑子有关,包括;10.7 cm射电通量,太阳总辐照度,磁场,耀斑和日冕物质抛射,地磁活动,银河系宇宙射线通量,以及树木年轮和冰芯中的放射性同位素。单个太阳活动周期的特征包括最大值和最小值、周期周期和振幅、周期形状、活动纬度的赤道漂移、半球不对称性和活动经度。周期到周期的变异性包括蒙德极小期、格莱斯伯格周期和格内维舍夫-奥尔(奇偶)规则。短期变率包括154天周期、准两年变化和双峰最大值。最后,我们对太阳周期的预测技术进行了检验,并对太阳周期23和24进行了更仔细的研究。
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引用次数: 595
Evolution of Active Regions 活动区演化
IF 20.9 1区 物理与天体物理 Pub Date : 2015-09-09 DOI: 10.1007/lrsp-2015-1
Lidia van Driel-Gesztelyi, Lucie May Green

The evolution of active regions (AR) from their emergence through their long decay process is of fundamental importance in solar physics. Since large-scale flux is generated by the deep-seated dynamo, the observed characteristics of flux emergence and that of the subsequent decay provide vital clues as well as boundary conditions for dynamo models. Throughout their evolution, ARs are centres of magnetic activity, with the level and type of activity phenomena being dependent on the evolutionary stage of the AR. As new flux emerges into a pre-existing magnetic environment, its evolution leads to re-configuration of small-and large-scale magnetic connectivities. The decay process of ARs spreads the once-concentrated magnetic flux over an ever-increasing area. Though most of the flux disappears through small-scale cancellation processes, it is the remnant of large-scale AR fields that is able to reverse the polarity of the poles and build up new polar fields. In this Living Review the emphasis is put on what we have learned from observations, which is put in the context of modelling and simulation efforts when interpreting them. For another, modelling-focused Living Review on the sub-surface evolution and emergence of magnetic flux see Fan (2009). In this first version we focus on the evolution of dominantly bipolar ARs.

活动区(AR)从它们的出现到它们漫长的衰变过程的演化在太阳物理学中具有重要的基础意义。由于大尺度磁通是由深层发电机产生的,观测到的磁通出现和随后的衰减特征为发电机模型提供了重要的线索和边界条件。在整个演化过程中,AR是磁活动的中心,活动现象的水平和类型取决于AR的演化阶段。当新的通量出现在预先存在的磁环境中时,其演化导致小型和大型磁连通性的重新配置。ARs的衰变过程将曾经集中的磁通量扩散到一个不断增加的区域。虽然大部分通量通过小规模的抵消过程消失,但它是大规模AR场的残余,能够逆转两极的极性并建立新的极地场。在这篇生活评论中,重点放在我们从观察中学到的东西上,这是在解释它们时在建模和模拟努力的背景下进行的。另一方面,以模拟为重点的关于地下磁通演化和出现的《生活评论》(Living Review)见Fan(2009)。在第一个版本中,我们主要关注双相ar的演变。
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引用次数: 169
The FIP and Inverse FIP Effects in Solar and Stellar Coronae 太阳和恒星日冕中的FIP和逆FIP效应
IF 20.9 1区 物理与天体物理 Pub Date : 2015-09-09 DOI: 10.1007/lrsp-2015-2
J. Martin Laming

We review our state of knowledge of coronal element abundance anomalies in the Sun and stars. We concentrate on the first ionization potential (FIP) effect observed in the solar corona and slow-speed wind, and in the coronae of solar-like dwarf stars, and the “inverse FIP” effect seen in the corona of stars of later spectral type; specifically M dwarfs. These effects relate to the enhancement or depletion, respectively, in coronal abundance with respect to photospheric values of elements with FIP below about 10 eV. They are interpreted in terms of the ponderomotive force due to the propagation and/or reflection of magnetohydrodynamic waves in the chromosphere. This acts on chromospheric ions, but not neutrals, and so can lead to ion-neutral fractionation.

A detailed description of the model applied to closed magnetic loops, and to open field regions is given, accounting for the observed difference in solar FIP fractionation between the slow and fast wind. It is shown that such a model can also account for the observed depletion of helium in the solar wind. The helium depletion is sensitive to the chromospheric altitude where ion-neutral separation occurs, and the behavior of the helium abundance in the closed magnetic loop strongly suggests that the waves have a coronal origin. This, and other similar inferences may be expected to have a strong bearing on theories of solar coronal heating.

Chromospheric waves originating from below as acoustic waves mode convert, mainly to fast-mode waves, can also give rise to ion-neutral separation. Depending on the geometry of the magnetic field, this can result in FIP or Inverse FIP effects. We argue that such configurations are more likely to occur in later-type stars (known to have stronger field in any case), and that this explains the occurrence of the Inverse FIP effect in M dwarfs. We conclude with a discussion of possible directions for future work.

我们回顾了我们对太阳和恒星中日冕元素丰度异常的认识状态。我们重点研究了在太阳日冕和慢速风以及类太阳矮星日冕中观测到的第一电离势(FIP)效应,以及在后期光谱型恒星日冕中观测到的“逆FIP”效应;特别是M个矮星。这些影响分别与相对于FIP低于约10 eV的元素的光球值的日冕丰度的增强或耗尽有关。它们被解释为由于磁流体动力波在色球中的传播和/或反射而产生的质动势。这作用于色球离子,而不是中性离子,因此可以导致离子中性分馏。考虑到观测到的太阳慢风和快风的FIP分值的差异,给出了该模型应用于闭合磁环和开放磁场区域的详细描述。结果表明,这种模型也可以解释观测到的太阳风中氦的耗尽。氦耗尽对离子中性分离发生的色球高度敏感,封闭磁环中氦丰度的行为强烈表明波具有日冕起源。这个和其他类似的推论可能会对太阳日冕加热理论产生强烈的影响。从下面发出的色球波作为声波模式转换,主要是快速模式波,也可以引起离子中性分离。根据磁场的几何形状,这可能导致FIP或逆FIP效应。我们认为,这种结构更可能发生在较晚类型的恒星(无论如何都有更强的场),这解释了M矮星中出现逆FIP效应的原因。最后,我们讨论了未来工作的可能方向。
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引用次数: 213
Large-scale Globally Propagating Coronal Waves. 大规模全球传播的日冕波。
IF 20.9 1区 物理与天体物理 Pub Date : 2015-01-01 Epub Date: 2015-12-30 DOI: 10.12942/lrsp-2015-3
Alexander Warmuth

Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging.

自20世纪60年代以来,在太阳色球层和日冕中观测到大规模的、全球传播的波状扰动。然而,对这些现象的详细分析直到20世纪90年代末才开始进行。这是由于来自许多太空仪器的高节奏日冕成像数据的可用性,这些数据经常显示壮观的全球传播的明亮锋面。这些扰动通常被称为日冕波,现在已经在广泛的光谱通道中被观测到,产生了丰富的信息。许多发现支持了对这些扰动的“经典”解释:在日冕中传播的快模MHD波或冲击。然而,似乎与这一图景不一致的观测结果刺激了另一种模型的发展,在这种模型中,“伪波”是由不断扩大的日冕物质抛射框架中的磁重构产生的。这导致了关于这些扰动的物理性质的激烈辩论。这篇综述的重点是展示过去15年的大量观测发现如何用于约束我们的大尺度日冕波模型,以及如何最终出现对这些扰动的连贯物理理解。
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引用次数: 0
Flux Emergence (Theory) 通量涌现(理论)
IF 20.9 1区 物理与天体物理 Pub Date : 2014-07-17 DOI: 10.12942/lrsp-2014-3
Mark C. M. Cheung, Hiroaki Isobe

Magnetic flux emergence from the solar convection zone into the overlying atmosphere is the driver of a diverse range of phenomena associated with solar activity. In this article, we introduce theoretical concepts central to the study of flux emergence and discuss how the inclusion of different physical effects (e.g., magnetic buoyancy, magnetoconvection, reconnection, magnetic twist, interaction with ambient field) in models impact the evolution of the emerging field and plasma.

从太阳对流区进入上覆大气的磁通量是一系列与太阳活动有关的现象的驱动因素。在这篇文章中,我们介绍了磁涌现研究的核心理论概念,并讨论了在模型中包含不同的物理效应(例如,磁浮力、磁对流、重联、磁扭曲、与环境场的相互作用)如何影响新兴场和等离子体的演变。
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引用次数: 151
Infrared Solar Physics 红外太阳物理学
IF 20.9 1区 物理与天体物理 Pub Date : 2014-03-21 DOI: 10.12942/lrsp-2014-2
Matthew J. Penn

The infrared solar spectrum contains a wealth of physical data about our Sun, and is explored using modern detectors and technology with new ground-based solar telescopes. The scientific motivation behind exploring these wavelengths is presented, along with a brief look at the rich history of observations here. Several avenues of solar physics research exploiting and benefiting from observations at infrared wavelengths from roughly 1000 nm to 12 400 nm are discussed, and the instrument and detector technology driving this research is briefly summarized. Finally, goals for future work at infrared wavelengths are presented in conjunction with ground and space-based observations.

太阳红外光谱包含了大量关于太阳的物理数据,并使用现代探测器和技术与新的地面太阳望远镜进行了探索。本文介绍了探索这些波长背后的科学动机,并简要介绍了这里丰富的观测历史。讨论了利用1000 ~ 12 400 nm红外波段观测的几种太阳物理研究途径,并简要总结了推动这一研究的仪器和探测器技术。最后,结合地面和天基观测,提出了未来红外波长工作的目标。
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引用次数: 55
期刊
Living Reviews in Solar Physics
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