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Coronal Mass Ejections: Observations 日冕物质抛射:观测
IF 20.9 1区 物理与天体物理 Pub Date : 2012-06-29 DOI: 10.12942/lrsp-2012-3
David F. Webb, Timothy A. Howard

Solar eruptive phenomena embrace a variety of eruptions, including flares, solar energetic particles, and radio bursts. Since the vast majority of these are associated with the eruption, development, and evolution of coronal mass ejections (CMEs), we focus on CME observations in this review. CMEs are a key aspect of coronal and interplanetary dynamics. They inject large quantities of mass and magnetic flux into the heliosphere, causing major transient disturbances. CMEs can drive interplanetary shocks, a key source of solar energetic particles and are known to be the major contributor to severe space weather at the Earth. Studies over the past decade using the data sets from (among others) the SOHO, TRACE, Wind, ACE, STEREO, and SDO spacecraft, along with ground-based instruments, have improved our knowledge of the origins and development of CMEs at the Sun and how they contribute to space weather at Earth. SOHO, launched in 1995, has provided us with almost continuous coverage of the solar corona over more than a complete solar cycle, and the heliospheric imagers SMEI (2003–2011) and the HIs (operating since early 2007) have provided us with the capability to image and track CMEs continually across the inner heliosphere. We review some key coronal properties of CMEs, their source regions and their propagation through the solar wind. The LASCO coronagraphs routinely observe CMEs launched along the Sun-Earth line as halo-like brightenings. STEREO also permits observing Earth-directed CMEs from three different viewpoints of increasing azimuthal separation, thereby enabling the estimation of their three-dimensional properties. These are important not only for space weather prediction purposes, but also for understanding the development and internal structure of CMEs since we view their source regions on the solar disk and can measure their in-situ characteristics along their axes. Included in our discussion of the recent developments in CME-related phenomena are the latest developments from the STEREO and LASCO coronagraphs and the SMEI and HI heliospheric imagers.

太阳爆发现象包括各种各样的爆发,包括耀斑、太阳高能粒子和射电爆发。由于其中绝大多数都与日冕物质抛射(CME)的喷发、发展和演化有关,因此本文将重点介绍CME的观测结果。日冕物质抛射是日冕和行星际动力学的一个关键方面。它们向日球层注入大量质量和磁通量,造成重大的瞬态扰动。日冕物质抛射可以驱动行星际冲击,这是太阳高能粒子的主要来源,也是造成地球恶劣太空天气的主要原因。在过去的十年中,利用SOHO、TRACE、Wind、ACE、STEREO和SDO航天器以及地面仪器的数据集进行的研究,提高了我们对太阳日冕物质抛射的起源和发展以及它们如何影响地球空间天气的认识。SOHO于1995年发射,为我们提供了超过一个完整太阳周期的日冕几乎连续的覆盖,日球层成像仪SMEI(2003-2011)和he(自2007年初开始运行)为我们提供了在内日球层连续成像和跟踪cme的能力。我们回顾了日冕物质抛射的一些关键的日冕性质,它们的来源区域和它们在太阳风中的传播。LASCO日冕仪定期观测沿日地线发射的日冕物质抛射,形成类似光晕的光亮。STEREO还允许从三个不同的角度观察地球方向的日冕物质抛射,从而增加方位角分离,从而能够估计它们的三维特性。这不仅对空间天气预报很重要,而且对了解日冕物质抛射的发展和内部结构也很重要,因为我们可以在太阳盘中看到它们的来源区域,并可以沿着它们的轴线测量它们的原位特征。在我们对日冕物质抛射相关现象的最新进展的讨论中,包括来自STEREO和LASCO日冕仪以及SMEI和HI日球成像仪的最新进展。
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引用次数: 485
Prominence Oscillations 突出振荡
IF 20.9 1区 物理与天体物理 Pub Date : 2012-04-05 DOI: 10.12942/lrsp-2012-2
Iñigo Arregui, Ramón Oliver, José Luis Ballester

Prominences are intriguing, but poorly understood, magnetic structures of the solar corona. The dynamics of solar prominences has been the subject of a large number of studies, and of particular interest is the study of prominence oscillations. Ground- and space-based observations have confirmed the presence of oscillatory motions in prominences and they have been interpreted in terms of magnetohydrodynamic (MHD) waves. This interpretation opens the door to perform prominence seismology, whose main aim is to determine physical parameters in magnetic and plasma structures (prominences) that are difficult to measure by direct means. Here, we review the observational information gathered about prominence oscillations as well as the theoretical models developed to interpret small amplitude oscillations and their temporal and spatial attenuation. Finally, several prominence seismology applications are presented.

日珥很有趣,但人们对日冕的磁性结构知之甚少。太阳日珥的动力学一直是大量研究的主题,特别有趣的是日珥振荡的研究。地面和空间观测已经证实了日珥中振荡运动的存在,它们已经用磁流体动力学(MHD)波来解释。这一解释为日珥地震学的研究打开了大门,其主要目的是确定难以直接测量的磁和等离子体结构(日珥)的物理参数。在此,我们回顾了日珥振荡的观测资料,以及用来解释小振幅振荡及其时空衰减的理论模型。最后,介绍了几个突出地震的应用。
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引用次数: 82
Coronal Mass Ejections: Models and Their Observational Basis 日冕物质抛射:模型及其观测基础
IF 20.9 1区 物理与天体物理 Pub Date : 2011-04-08 DOI: 10.12942/lrsp-2011-1
P. F. Chen

Coronal mass ejections (CMEs) are the largest-scale eruptive phenomenon in the solar system, expanding from active region-sized nonpotential magnetic structure to a much larger size. The bulk of plasma with a mass of ~ 1011,1013 kg is hauled up all the way out to the interplanetary space with a typical velocity of several hundred or even more than 1000 km s?1, with a chance to impact our Earth, resulting in hazardous space weather conditions. They involve many other much smaller-sized solar eruptive phenomena, such as X-ray sigmoids, filament/prominence eruptions, solar flares, plasma heating and radiation, particle acceleration, EIT waves, EUV dimmings, Moreton waves, solar radio bursts, and so on. It is believed that, by shedding the accumulating magnetic energy and helicity, they complete the last link in the chain of the cycling of the solar magnetic field. In this review, I try to explicate our understanding on each stage of the fantastic phenomenon, including their pre-eruption structure, their triggering mechanisms and the precursors indicating the initiation process, their acceleration and propagation. Particular attention is paid to clarify some hot debates, e.g., whether magnetic reconnection is necessary for the eruption, whether there are two types of CMEs, how the CME frontal loop is formed, and whether halo CMEs are special.

日冕物质抛射(CMEs)是太阳系中规模最大的喷发现象,从活动区域大小的非势磁结构扩展到更大的规模。质量约为1011,1013 kg的等离子体以典型的几百甚至超过1000 km / s的速度被一路拖到行星际空间。1、有机会撞击我们的地球,导致危险的太空天气状况。它们涉及许多其他较小规模的太阳爆发现象,如x射线s型流、灯丝/日珥喷发、太阳耀斑、等离子体加热和辐射、粒子加速、EIT波、EUV变暗、摩尔顿波、太阳射电暴等等。据信,通过释放积累的磁能和螺旋度,它们完成了太阳磁场循环链条的最后一环。在本文中,我试图阐述我们对奇异现象的每个阶段的理解,包括它们的爆发前结构,它们的触发机制以及它们的开始过程的前兆,它们的加速和传播。重点澄清了日冕物质抛射是否需要磁重联、是否有两种类型的日冕物质抛射、日冕物质抛射锋面环如何形成、日冕物质抛射是否特殊等热点问题。
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引用次数: 546
The Sun’s Supergranulation 太阳的超颗粒
IF 20.9 1区 物理与天体物理 Pub Date : 2010-12-01 DOI: 10.12942/lrsp-2010-2
Michel Rieutord, François Rincon

The Sun’s supergranulation refers to a physical pattern covering the surface of the quiet Sun with a typical horizontal scale of approximately 30,000 km and a lifetime of around 1.8 d. Its most noticeable observable signature is as a fluctuating velocity field of 360 m st-1 rms whose components are mostly horizontal. Supergranulation was discovered more than fifty years ago, however explaining why and how it originates still represents one of the main challenges of modern solar physics.

A lot of work has been devoted to the subject over the years, but observational constraints, conceptual difficulties and numerical limitations have all concurred to prevent a detailed understanding of the supergranulation phenomenon so far. With the advent of 21st century supercomputing resources and the availability of unprecedented high-resolution observations of the Sun, a stage at which key progress can be made has now been reached. A unifying strategy between observations and modelling is more than ever required for this to be possible.

The primary aim of this review is therefore to provide readers with a detailed interdisciplinary description of past and current research on the problem, from the most elaborate observational strategies to recent theoretical and numerical modelling efforts that have all taken up the challenge of uncovering the origins of supergranulation. Throughout the text, we attempt to pick up the most robust findings so far, but we also outline the difficulties, limitations and open questions that the community has been confronted with over the years.

In the light of the current understanding of the multiscale dynamics of the quiet photosphere, we finally suggest a tentative picture of supergranulation as a dynamical feature of turbulent magnetohydrodynamic convection in an extended spatial domain, with the aim of stimulating future research and discussions.

太阳的超粒是指覆盖在安静太阳表面的物理模式,其典型的水平尺度约为30,000公里,寿命约为1.8 d。其最显著的可观测特征是360 m st-1 rms的波动速度场,其组成部分主要是水平的。超粒现象早在50多年前就被发现了,然而解释它的起源和原因仍然是现代太阳物理学的主要挑战之一。多年来,人们对这个问题进行了大量的研究,但迄今为止,观测上的限制、概念上的困难和数值上的限制都阻碍了对超粒现象的详细理解。随着21世纪超级计算资源的出现和对太阳前所未有的高分辨率观测的可用性,现在已经达到了可以取得关键进展的阶段。观测和建模之间的统一策略比以往任何时候都更有可能实现。因此,本综述的主要目的是为读者提供过去和当前对该问题的研究的详细跨学科描述,从最详细的观察策略到最近的理论和数值模拟努力,这些努力都接受了揭示超颗粒起源的挑战。在整个文本中,我们试图挑选迄今为止最有力的发现,但我们也概述了困难,限制和开放的问题,该社区多年来一直面临。根据目前对安静光球的多尺度动力学的理解,我们最后提出了超颗粒作为湍流磁流体动力对流在扩展空间域中的动力学特征的初步图景,旨在促进未来的研究和讨论。
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引用次数: 143
Space Weather: The Solar Perspective 太空天气:太阳的视角
IF 20.9 1区 物理与天体物理 Pub Date : 2006-12-01 DOI: 10.12942/lrsp-2006-2
Rainer Schwenn

The term space weather refers to conditions on the Sun and in the solar wind, magnetosphere, ionosphere, and thermosphere that can influence the performance and reliability of space-borne and ground-based technological systems and that can affect human life and health. Our modern hi-tech society has become increasingly vulnerable to disturbances from outside the Earth system, in particular to those initiated by explosive events on the Sun: Flares release flashes of radiation that can heat up the terrestrial atmosphere such that satellites are slowed down and drop into lower orbits, solar energetic particles accelerated to near-relativistic energies may endanger astronauts traveling through interplanetary space, and coronal mass ejections are gigantic clouds of ionized gas ejected into interplanetary space that after a few hours or days may hit the Earth and cause geomagnetic storms. In this review, I describe the several chains of actions originating in our parent star, the Sun, that affect Earth, with particular attention to the solar phenomena and the subsequent effects in interplanetary space.

空间天气一词是指太阳和太阳风、磁层、电离层和热层中能够影响星载和地面技术系统的性能和可靠性并能够影响人类生命和健康的条件。我们的现代高科技社会越来越容易受到来自地球系统外的干扰,特别是那些由太阳爆炸事件引发的干扰。耀斑释放出的辐射会使地球大气升温,从而使卫星减速并落入较低的轨道;太阳高能粒子加速到接近相对论的能量,可能危及在行星际空间旅行的宇航员;日冕物质抛射是被抛射到行星际空间的巨大电离气体云,在几小时或几天后可能撞击地球并引起地磁风暴。在这篇综述中,我描述了起源于我们的母星太阳的影响地球的几条行动链,特别关注太阳现象及其对行星际空间的后续影响。
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引用次数: 388
Large-Scale Dynamics of the Convection Zone and Tachocline 对流区和速斜的大尺度动力学
IF 20.9 1区 物理与天体物理 Pub Date : 2005-12-01 DOI: 10.12942/lrsp-2005-1
Mark S. Miesch

The past few decades have seen dramatic progress in our understanding of solar interior dynamics, prompted by the relatively new science of helioseismology and increasingly sophisticated numerical models. As the ultimate driver of solar variability and space weather, global-scale convective motions are of particular interest from a practical as well as a theoretical perspective. Turbulent convection under the influence of rotation and stratification redistributes momentum and energy, generating differential rotation, meridional circulation, and magnetic fields through hydromagnetic dynamo processes. In the solar tachocline near the base of the convection zone, strong angular velocity shear further amplifies fields which subsequently rise to the surface to form active regions. Penetrative convection, instabilities, stratified turbulence, and waves all add to the dynamical richness of the tachocline region and pose particular modeling challenges. In this article we review observational, theoretical, and computational investigations of global-scale dynamics in the solar interior. Particular emphasis is placed on high-resolution global simulations of solar convection, highlighting what we have learned from them and how they may be improved.

在过去的几十年里,我们对太阳内部动力学的理解取得了巨大的进步,这是由相对较新的日震学和日益复杂的数值模型所推动的。作为太阳变率和空间天气的最终驱动因素,全球尺度的对流运动从实践和理论的角度来看都是特别有趣的。在旋转和分层的影响下,湍流对流重新分配动量和能量,通过水力发电机过程产生微分旋转、经向环流和磁场。在靠近对流区底部的太阳速斜中,强角速度切变进一步放大了随后上升到地表形成活动区的场。穿透性对流、不稳定性、分层湍流和波浪都增加了速斜区域的动力丰富性,并提出了特殊的建模挑战。在这篇文章中,我们回顾了太阳内部全球尺度动力学的观测、理论和计算研究。特别强调的是太阳对流的高分辨率全球模拟,强调我们从中学到的东西以及如何改进它们。
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引用次数: 300
Local Helioseismology 当地日震学
IF 20.9 1区 物理与天体物理 Pub Date : 2005-12-01 DOI: 10.12942/lrsp-2005-6
Laurent Gizon, Aaron C. Birch

We review the current status of local helioseismology, covering both theoretical and observational results. After a brief introduction to solar oscillations and wave propagation through in-homogeneous media, we describe the main techniques of local helioseismology: Fourier-Hankel decomposition, ring-diagram analysis, time-distance helioseismology, helioseismic holography, and direct modeling. We discuss local helioseismology of large-scale flows, the solar-cycle dependence of these flows, perturbations associated with regions of magnetic activity, and solar supergranulation.

本文从理论和观测两方面综述了我国日震学的研究现状。在简要介绍了太阳振荡和波在非均匀介质中的传播之后,我们描述了局部日震学的主要技术:傅里叶-汉克尔分解、环图分析、时距日震学、日震全息术和直接建模。我们讨论了大尺度气流的局部日震学,这些气流的太阳周期依赖性,与磁活动区域相关的扰动,以及太阳超粒化。
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引用次数: 92
Coronal Waves and Oscillations 日冕波和振荡
IF 20.9 1区 物理与天体物理 Pub Date : 2005-05-07 DOI: 10.1017/S174392130600250X
V. Nakariakov, E. Verwichte
Wave and oscillatory activity of the solar corona is confidently observed with modern imaging and spectral instruments in the visible light, EUV, X-ray and radio bands, and interpreted in terms of magnetohydrodynamic (MHD) wave theory. The review reflects the current trends in the observational study of coronal waves and oscillations (standing kink, sausage and longitudinal modes, propagating slow waves and fast wave trains, the search for torsional waves), theoretical modelling of interaction of MHD waves with plasma structures, and implementation of the theoretical results for the mode identification. Also the use of MHD waves for remote diagnostics of coronal plasma — MHD coronal seismology — is discussed and the applicability of this method for the estimation of coronal magnetic field, transport coefficients, fine structuring and heating function is demonstrated.
利用现代成像和光谱仪器,在可见光、极紫外、x射线和无线电波段自信地观测到太阳日冕的波动和振荡活动,并根据磁流体动力学(MHD)波动理论进行了解释。综述了日冕波和振荡的观测研究(驻扭、香肠和纵模,传播慢波和快波列,寻找扭转波)、MHD波与等离子体结构相互作用的理论建模以及模式识别理论结果的实现等方面的最新趋势。讨论了MHD波在日冕等离子体远程诊断中的应用——MHD日冕地震学,并论证了该方法在估算日冕磁场、输运系数、精细结构和加热功能等方面的适用性。
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引用次数: 388
期刊
Living Reviews in Solar Physics
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