Living Reviews in Solar Physics最新文献_第3页

Global seismology of the Sun 全球太阳地震学

IF 20.9 1区物理与天体物理

Living Reviews in Solar Physics Pub Date : 2016-08-08 DOI: 10.1007/s41116-016-0003-4

Sarbani Basu

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

Living Reviews in Solar Physics Pub Date : 2016-07-05 DOI: 10.1007/s41116-016-0001-6

Carlos Allende Prieto

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

Living Reviews in Solar Physics Pub Date : 2015-12-01 DOI: 10.1007/lrsp-2015-6

Elena Khomenko, Manuel Collados

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

Living Reviews in Solar Physics Pub Date : 2015-12-01 DOI: 10.1007/lrsp-2015-8

Günter Houdek, Marc-Antoine Dupret

引用次数: 43

The Solar Cycle 太阳周期

IF 20.9 1区物理与天体物理

Living Reviews in Solar Physics Pub Date : 2015-09-21 DOI: 10.1007/lrsp-2015-4

David H. Hathaway

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

Living Reviews in Solar Physics Pub Date : 2015-09-09 DOI: 10.1007/lrsp-2015-1

Lidia van Driel-Gesztelyi, Lucie May Green

{"title":"Evolution of Active Regions","authors":"Lidia van Driel-Gesztelyi, Lucie May Green","doi":"10.1007/lrsp-2015-1","DOIUrl":"https://doi.org/10.1007/lrsp-2015-1","url":null,"abstract":"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.","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":"12 1","pages":""},"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

Living Reviews in Solar Physics Pub Date : 2015-09-09 DOI: 10.1007/lrsp-2015-2

J. Martin Laming

{"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":"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.","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":"12 1","pages":""},"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

Living Reviews in Solar Physics Pub Date : 2015-01-01 Epub Date: 2015-12-30 DOI: 10.12942/lrsp-2015-3

Alexander Warmuth

{"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":"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.","PeriodicalId":49147,"journal":{"name":"Living Reviews in Solar Physics","volume":"12 ","pages":"1-101"},"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

Living Reviews in Solar Physics Pub Date : 2014-07-17 DOI: 10.12942/lrsp-2014-3

Mark C. M. Cheung, Hiroaki Isobe

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

Living Reviews in Solar Physics Pub Date : 2014-03-21 DOI: 10.12942/lrsp-2014-2

Matthew J. Penn

引用次数: 55