LEADER 02270nam  2200409z- 450 
001 9910227347603321
005 20231214133403.0
035   $a(CKB)4100000000883857
035   $a(oapen)https://directory.doabooks.org/handle/20.500.12854/44090
035   $a(EXLCZ)994100000000883857
100   $a20202102d2017      |y             0
101 0 $aeng
135   $aurmn|---annan
181   $ctxt$2rdacontent
182   $cc$2rdamedia
183   $acr$2rdacarrier
200 10$aCoronal Magnetometry
210   $cFrontiers Media SA$d2017
215   $a1 electronic resource (172 p.)
225 1 $aFrontiers Research Topics
311   $a2-88945-220-4 
330   $aMagnetism defines the complex and dynamic solar corona. It determines the magnetic loop structure that dominates images of the corona, and stores the energy necessary to drive coronal eruptive phenomena and flare explosions. At great heights the corona transitions into the ever-outflowing solar wind, whose speed and three-dimensional morphology are controlled by the global coronal magnetic field. Coronal magnetism is thus at the heart of any understanding of the nature of the corona, and essential for predictive capability of how the Sun affects the Earth. Coronal magnetometry is a subject that requires a concerted effort to draw together the different strands of research happening around the world. Each method provides some information about the field, but none of them can be used to determine the full 3D field structure in the full volume of the corona. Thus, we need to combine them to understand the full picture. The purpose of this Frontiers Research Topic on Coronal Magnetometry is to provide a forum for comparing and coordinating these research methods, and for discussing future opportunities.
610   $asolar corona
610   $aSolar Activity
610   $amagnetohydrodynamics
610   $asolar flares
610   $aCoronal mass ejections
610   $aMagnetic Fields
610   $aspectropolarimetry
610   $aSun
700   $aLaurel A. Rachmeler$4auth$01304387
702   $aSarah E. Gibson$4auth
702   $aStephen M. White$4auth
906   $aBOOK
912   $a9910227347603321
996   $aCoronal Magnetometry$93027350
997   $aUNINA