{"title":"Coronal Waves and Oscillations","authors":"Valery M. Nakariakov, Erwin Verwichte","doi":"10.12942/lrsp-2005-3","DOIUrl":"https://doi.org/10.12942/lrsp-2005-3","url":null,"abstract":"<p>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.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":"2 1","pages":""},"PeriodicalIF":20.9,"publicationDate":"2005-05-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2005-3","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4630938","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}
{"title":"Magnetic Fields in the Solar Convection Zone","authors":"Yuhong Fan","doi":"10.12942/lrsp-2004-1","DOIUrl":"https://doi.org/10.12942/lrsp-2004-1","url":null,"abstract":"<p>Recent studies of the dynamic evolution of magnetic flux tubes in the solar convection zone are reviewed with focus on emerging flux tubes responsible for the formation of solar active regions. The current prevailing picture is that active regions on the solar surface originate from strong toroidal magnetic fields generated by the solar dynamo mechanism at the thin tachocline layer at the base of the solar convection zone. Thus the magnetic fields need to traverse the entire convection zone before they reach the photosphere to form the observed solar active regions. This review discusses results with regard to the following major topics:\u0000</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":"1 1","pages":""},"PeriodicalIF":20.9,"publicationDate":"2004-12-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2004-1","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4009924","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}
{"title":"Astrospheres and Solar-like Stellar Winds","authors":"Brian E. Wood","doi":"10.12942/lrsp-2004-2","DOIUrl":"https://doi.org/10.12942/lrsp-2004-2","url":null,"abstract":"<p>Stellar analogs for the solar wind have proven to be frustratingly difficult to detect directly. However, these stellar winds can be studied indirectly by observing the interaction regions carved out by the collisions between these winds and the interstellar medium (ISM). These interaction regions are called “astrospheres”, analogous to the “heliosphere” surrounding the Sun. The heliosphere and astrospheres contain a population of hydrogen heated by charge exchange processes that can produce enough H I Ly<i>α</i> absorption to be detectable in UV spectra of nearby stars from the <i>Hubble Space Telescope</i> (HST). The amount of astrospheric absorption is a diagnostic for the strength of the stellar wind, so these observations have provided the first measurements of solar-like stellar winds. Results from these stellar wind studies and their implications for our understanding of the solar wind are reviewed here. Of particular interest are results concerning the past history of the solar wind and its impact on planetary atmospheres.</p>","PeriodicalId":687,"journal":{"name":"Living Reviews in Solar Physics","volume":"1 1","pages":""},"PeriodicalIF":20.9,"publicationDate":"2004-07-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://sci-hub-pdf.com/10.12942/lrsp-2004-2","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5115571","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}
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