首页 > 最新文献

Living Reviews in Solar Physics最新文献

英文 中文
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。
{"title":"Oscillations and Waves in Sunspots","authors":"Elena Khomenko,&nbsp;Manuel Collados","doi":"10.1007/lrsp-2015-6","DOIUrl":"https://doi.org/10.1007/lrsp-2015-6","url":null,"abstract":"<p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2015-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1007/lrsp-2015-6","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4011980","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"Interaction Between Convection and Pulsation","authors":"Günter Houdek,&nbsp;Marc-Antoine Dupret","doi":"10.1007/lrsp-2015-8","DOIUrl":"https://doi.org/10.1007/lrsp-2015-8","url":null,"abstract":"<p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2015-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1007/lrsp-2015-8","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4013797","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"The Solar Cycle","authors":"David H. Hathaway","doi":"10.1007/lrsp-2015-4","DOIUrl":"https://doi.org/10.1007/lrsp-2015-4","url":null,"abstract":"<p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2015-09-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1007/lrsp-2015-4","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4846232","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"Evolution of Active Regions","authors":"Lidia van Driel-Gesztelyi,&nbsp;Lucie May Green","doi":"10.1007/lrsp-2015-1","DOIUrl":"https://doi.org/10.1007/lrsp-2015-1","url":null,"abstract":"<p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2015-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1007/lrsp-2015-1","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4404441","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"The FIP and Inverse FIP Effects in Solar and Stellar Coronae","authors":"J. Martin Laming","doi":"10.1007/lrsp-2015-2","DOIUrl":"https://doi.org/10.1007/lrsp-2015-2","url":null,"abstract":"<p>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.</p><p>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.</p><p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2015-09-09","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.1007/lrsp-2015-2","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4401288","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"Large-scale Globally Propagating Coronal Waves.","authors":"Alexander Warmuth","doi":"10.12942/lrsp-2015-3","DOIUrl":"https://doi.org/10.12942/lrsp-2015-3","url":null,"abstract":"<p><p>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. <i>Coronal waves</i>, 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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2015-01-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.ncbi.nlm.nih.gov/pmc/articles/PMC4944665/pdf/","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"34616816","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"Flux Emergence (Theory)","authors":"Mark C. M. Cheung,&nbsp;Hiroaki Isobe","doi":"10.12942/lrsp-2014-3","DOIUrl":"https://doi.org/10.12942/lrsp-2014-3","url":null,"abstract":"<p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2014-07-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2014-3","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4680883","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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。
{"title":"Infrared Solar Physics","authors":"Matthew J. Penn","doi":"10.12942/lrsp-2014-2","DOIUrl":"https://doi.org/10.12942/lrsp-2014-2","url":null,"abstract":"<p>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.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2014-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2014-2","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4827364","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 55
A History of Solar Activity over Millennia 太阳活动千年的历史
IF 20.9 1区 物理与天体物理 Pub Date : 2013-03-21 DOI: 10.12942/lrsp-2013-1
Ilya G. Usoskin

Presented here is a review of present knowledge of the long-term behavior of solar activity on a multi-millennial timescale, as reconstructed using the indirect proxy method. The concept of solar activity is discussed along with an overview of the special indices used to quantify different aspects of variable solar activity, with special emphasis upon sunspot number.

Over long timescales, quantitative information about past solar activity can only be obtained using a method based upon indirect proxies, such as the cosmogenic isotopes 14C and 10Be in natural stratified archives (e.g., tree rings or ice cores). We give an historical overview of the development of the proxy-based method for past solar-activity reconstruction over millennia, as well as a description of the modern state. Special attention is paid to the verification and cross-calibration of reconstructions. It is argued that this method of cosmogenic isotopes makes a solid basis for studies of solar variability in the past on a long timescale (centuries to millennia) during the Holocene.

A separate section is devoted to reconstructions of strong solar energetic-particle (SEP) events in the past, that suggest that the present-day average SEP flux is broadly consistent with estimates on longer timescales, and that the occurrence of extra-strong events is unlikely.

Finally, the main features of the long-term evolution of solar magnetic activity, including the statistics of grand minima and maxima occurrence, are summarized and their possible implications, especially for solar/stellar dynamo theory, are discussed.

本文介绍了利用间接代理方法重建的几千年时间尺度上太阳活动的长期行为的现有知识。讨论了太阳活动的概念,并概述了用于量化可变太阳活动不同方面的特殊指数,特别强调了太阳黑子数。在长时间尺度上,关于过去太阳活动的定量信息只能通过基于间接代理的方法获得,例如自然分层档案(如树轮或冰芯)中的宇宙成因同位素14C和10Be。我们对几千年来基于代理的太阳活动重建方法的发展进行了历史概述,并对现代状态进行了描述。特别注意重建的验证和交叉校准。有人认为,这种宇宙成因同位素的方法为在全新世期间研究过去很长时间尺度(几百到几千年)的太阳变化奠定了坚实的基础。一个单独的部分专门用于重建过去的强太阳能量粒子(SEP)事件,这表明,目前的平均SEP通量与较长时间尺度上的估计大致一致,并且超强事件的发生是不可能的。最后,总结了太阳磁活动长期演变的主要特征,包括极大极小期和极大极小期的统计数据,并讨论了它们可能的意义,特别是对太阳/恒星发电机理论的意义。
{"title":"A History of Solar Activity over Millennia","authors":"Ilya G. Usoskin","doi":"10.12942/lrsp-2013-1","DOIUrl":"https://doi.org/10.12942/lrsp-2013-1","url":null,"abstract":"<p>Presented here is a review of present knowledge of the long-term behavior of solar activity on a multi-millennial timescale, as reconstructed using the indirect proxy method. The concept of solar activity is discussed along with an overview of the special indices used to quantify different aspects of variable solar activity, with special emphasis upon sunspot number.</p><p>Over long timescales, quantitative information about past solar activity can only be obtained using a method based upon indirect proxies, such as the cosmogenic isotopes <sup>14</sup>C and <sup>10</sup>Be in natural stratified archives (e.g., tree rings or ice cores). We give an historical overview of the development of the proxy-based method for past solar-activity reconstruction over millennia, as well as a description of the modern state. Special attention is paid to the verification and cross-calibration of reconstructions. It is argued that this method of cosmogenic isotopes makes a solid basis for studies of solar variability in the past on a long timescale (centuries to millennia) during the Holocene.</p><p>A separate section is devoted to reconstructions of strong solar energetic-particle (SEP) events in the past, that suggest that the present-day average SEP flux is broadly consistent with estimates on longer timescales, and that the occurrence of extra-strong events is unlikely.</p><p>Finally, the main features of the long-term evolution of solar magnetic activity, including the statistics of grand minima and maxima occurrence, are summarized and their possible implications, especially for solar/stellar dynamo theory, are discussed.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2013-03-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2013-1","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4827335","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 265
The Sun’s Global Photospheric and Coronal Magnetic Fields: Observations and Models 太阳的全球光球和日冕磁场:观测和模型
IF 20.9 1区 物理与天体物理 Pub Date : 2012-11-26 DOI: 10.12942/lrsp-2012-6
Duncan H. Mackay, Anthony R. Yeates

In this review, our present day understanding of the Sun’s global photospheric and coronal magnetic fields is discussed from both observational and theoretical viewpoints. Firstly, the large-scale properties of photospheric magnetic fields are described, along with recent advances in photospheric magnetic flux transport models. Following this, the wide variety of theoretical models used to simulate global coronal magnetic fields are described. From this, the combined application of both magnetic flux transport simulations and coronal modeling techniques to describe the phenomena of coronal holes, the Sun’s open magnetic flux and the hemispheric pattern of solar filaments is discussed. Finally, recent advances in non-eruptive global MHD models are described. While the review focuses mainly on solar magnetic fields, recent advances in measuring and modeling stellar magnetic fields are described where appropriate. In the final section key areas of future research are identified.

在这篇综述中,我们从观测和理论两个角度讨论了我们目前对太阳全球光球和日冕磁场的认识。首先介绍了光球磁场的大尺度特性,以及光球磁通量输运模型的最新进展。在此之后,描述了用于模拟全球日冕磁场的各种理论模型。在此基础上,讨论了磁通量输运模拟和日冕模拟技术在日冕空穴、太阳开放磁通量和太阳细丝半球分布等现象中的联合应用。最后,介绍了非喷发型全球MHD模型的最新进展。虽然审查主要集中在太阳磁场,但在适当的地方描述了测量和模拟恒星磁场的最新进展。在最后一节,确定了未来研究的关键领域。
{"title":"The Sun’s Global Photospheric and Coronal Magnetic Fields: Observations and Models","authors":"Duncan H. Mackay,&nbsp;Anthony R. Yeates","doi":"10.12942/lrsp-2012-6","DOIUrl":"https://doi.org/10.12942/lrsp-2012-6","url":null,"abstract":"<p>In this review, our present day understanding of the Sun’s global photospheric and coronal magnetic fields is discussed from both observational and theoretical viewpoints. Firstly, the large-scale properties of photospheric magnetic fields are described, along with recent advances in photospheric magnetic flux transport models. Following this, the wide variety of theoretical models used to simulate global coronal magnetic fields are described. From this, the combined application of both magnetic flux transport simulations and coronal modeling techniques to describe the phenomena of coronal holes, the Sun’s open magnetic flux and the hemispheric pattern of solar filaments is discussed. Finally, recent advances in non-eruptive global MHD models are described. While the review focuses mainly on solar magnetic fields, recent advances in measuring and modeling stellar magnetic fields are described where appropriate. In the final section key areas of future research are identified.</p>","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":null,"pages":null},"PeriodicalIF":20.9,"publicationDate":"2012-11-26","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2012-6","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5014310","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":1,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
引用次数: 164
期刊
Living Reviews in Solar Physics
全部 Acc. Chem. Res. ACS Applied Bio Materials ACS Appl. Electron. Mater. ACS Appl. Energy Mater. ACS Appl. Mater. Interfaces ACS Appl. Nano Mater. ACS Appl. Polym. Mater. ACS BIOMATER-SCI ENG ACS Catal. ACS Cent. Sci. ACS Chem. Biol. ACS Chemical Health & Safety ACS Chem. Neurosci. ACS Comb. Sci. ACS Earth Space Chem. ACS Energy Lett. ACS Infect. Dis. ACS Macro Lett. ACS Mater. Lett. ACS Med. Chem. Lett. ACS Nano ACS Omega ACS Photonics ACS Sens. ACS Sustainable Chem. Eng. ACS Synth. Biol. Anal. Chem. BIOCHEMISTRY-US Bioconjugate Chem. BIOMACROMOLECULES Chem. Res. Toxicol. Chem. Rev. Chem. Mater. CRYST GROWTH DES ENERG FUEL Environ. Sci. Technol. Environ. Sci. Technol. Lett. Eur. J. Inorg. Chem. IND ENG CHEM RES Inorg. Chem. J. Agric. Food. Chem. J. Chem. Eng. Data J. Chem. Educ. J. Chem. Inf. Model. J. Chem. Theory Comput. J. Med. Chem. J. Nat. Prod. J PROTEOME RES J. Am. Chem. Soc. LANGMUIR MACROMOLECULES Mol. Pharmaceutics Nano Lett. Org. Lett. ORG PROCESS RES DEV ORGANOMETALLICS J. Org. Chem. J. Phys. Chem. J. Phys. Chem. A J. Phys. Chem. B J. Phys. Chem. C J. Phys. Chem. Lett. Analyst Anal. Methods Biomater. Sci. Catal. Sci. Technol. Chem. Commun. Chem. Soc. Rev. CHEM EDUC RES PRACT CRYSTENGCOMM Dalton Trans. Energy Environ. Sci. ENVIRON SCI-NANO ENVIRON SCI-PROC IMP ENVIRON SCI-WAT RES Faraday Discuss. Food Funct. Green Chem. Inorg. Chem. Front. Integr. Biol. J. Anal. At. Spectrom. J. Mater. Chem. A J. Mater. Chem. B J. Mater. Chem. C Lab Chip Mater. Chem. Front. Mater. Horiz. MEDCHEMCOMM Metallomics Mol. Biosyst. Mol. Syst. Des. Eng. Nanoscale Nanoscale Horiz. Nat. Prod. Rep. New J. Chem. Org. Biomol. Chem. Org. Chem. Front. PHOTOCH PHOTOBIO SCI PCCP Polym. Chem.
×
引用
GB/T 7714-2015
复制
MLA
复制
APA
复制
导出至
BibTeX EndNote RefMan NoteFirst NoteExpress
×
0
微信
客服QQ
Book学术公众号 扫码关注我们
反馈
×
意见反馈
请填写您的意见或建议
请填写您的手机或邮箱
×
提示
您的信息不完整,为了账户安全,请先补充。
现在去补充
×
提示
您因"违规操作"
具体请查看互助需知
我知道了
×
提示
现在去查看 取消
×
提示
确定
Book学术官方微信
Book学术文献互助
Book学术文献互助群
群 号:481959085
Book学术
文献互助 智能选刊 最新文献 互助须知 联系我们:info@booksci.cn
Book学术提供免费学术资源搜索服务,方便国内外学者检索中英文文献。致力于提供最便捷和优质的服务体验。
Copyright © 2023 Book学术 All rights reserved.
ghs 京公网安备 11010802042870号 京ICP备2023020795号-1