Coronal observations of CMEs

dc.creatorSchwenn, R
dc.creatorRaymond, JC
dc.creatorAlexander, D
dc.creatorCiaravella, A
dc.creatorGopalswamy, N
dc.creatorHoward, R
dc.creatorHudson, H
dc.creatorKaufmann, P
dc.creatorKlassen, A
dc.creatorMaia, D
dc.creatorMunoz-Martinez, G
dc.creatorPick, M
dc.creatorReiner, M
dc.creatorSrivastava, N
dc.creatorTripathi, D
dc.creatorVourlidas, A
dc.creatorWang, YM
dc.creatorZhang, J
dc.date2006
dc.dateMAR
dc.date2014-11-16T12:37:48Z
dc.date2015-11-26T16:22:45Z
dc.date2014-11-16T12:37:48Z
dc.date2015-11-26T16:22:45Z
dc.date.accessioned2018-03-28T23:04:12Z
dc.date.available2018-03-28T23:04:12Z
dc.identifierSpace Science Reviews. Springer, v. 123, n. 41699, n. 127, n. 176, 2006.
dc.identifier0038-6308
dc.identifierWOS:000242328400010
dc.identifier10.1007/s11214-006-9016-y
dc.identifierhttp://www.repositorio.unicamp.br/jspui/handle/REPOSIP/57225
dc.identifierhttp://www.repositorio.unicamp.br/handle/REPOSIP/57225
dc.identifierhttp://repositorio.unicamp.br/jspui/handle/REPOSIP/57225
dc.identifier.urihttp://repositorioslatinoamericanos.uchile.cl/handle/2250/1268147
dc.descriptionCMEs have been observed for over 30 years with a wide variety of instruments. It is now possible to derive detailed and quantitative information on CME morphology, velocity, acceleration and mass. Flares associated with CMEs are observed in X-rays, and several different radio signatures are also seen. Optical and UV spectra of CMEs both on the disk and at the limb provide velocities along the line of sight and diagnostics for temperature, density and composition. From the vast quantity of data we attempt to synthesize the current state of knowledge of the properties of CMEs, along with some specific observed characteristics that illuminate the physical processes occurring during CME eruption. These include the common three-part structures of CMEs, which is generally attributed to compressed material at the leading edge, a low-density magnetic bubble and dense prominence gas. Signatures of shock waves are seen, but the location of these shocks relative to the other structures and the occurrence rate at the heights where Solar Energetic Particles are produced remains controversial. The relationships among CMEs, Moreton waves, EIT waves, and EUV dimming are also cloudy. The close connection between CMEs and flares suggests that magnetic reconnection plays an important role in CME eruption and evolution. We discuss the evidence for reconnection in current sheets from white-light, X-ray, radio and UV observations. Finally, we summarize the requirements for future instrumentation that might answer the outstanding questions and the opportunities that new space-based and ground-based observatories will provide in the future.
dc.description123
dc.description41699
dc.description127
dc.description176
dc.languageen
dc.publisherSpringer
dc.publisherDordrecht
dc.publisherHolanda
dc.relationSpace Science Reviews
dc.relationSpace Sci. Rev.
dc.rightsfechado
dc.rightshttp://www.springer.com/open+access/authors+rights?SGWID=0-176704-12-683201-0
dc.sourceWeb of Science
dc.subjectsolar corona
dc.subjecteruptive prominences
dc.subjectcoronal mass ejections (CMEs)
dc.subjectflares
dc.subjectsolar wind
dc.subjectsolarmagnetic field
dc.subjectmagnetic reconnection
dc.subjectinterplanetary shock waves
dc.subjectICMEs
dc.subjectspace weather
dc.subjectsolar energetic particles (SEPs)
dc.subjectradio bursts
dc.subjectSelf-similar Magnetohydrodynamics
dc.subjectEjection-associated Shock
dc.subjectDuration Solar-flare
dc.subjectWhite-light Images
dc.subjectWhole Sun Month
dc.subjectX-ray Sources
dc.subjectMass Ejections
dc.subjectMagnetic Reconnection
dc.subjectEruptive Prominence
dc.subjectActive-region
dc.titleCoronal observations of CMEs
dc.typeArtículos de revistas


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