Coronal observations of CMEs : Report of working group A

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dc.contributor.authorSchwenn R.
dc.contributor.authorRaymond J.C.
dc.contributor.authorAlexander D.
dc.contributor.authorCiaravella A.
dc.contributor.authorGopalswamy N.
dc.contributor.authorHoward R.
dc.contributor.authorHudson H.
dc.contributor.authorKaufmann P.
dc.contributor.authorKlassen A.
dc.contributor.authorMaia D.
dc.contributor.authorMunoz-Martinez G.
dc.contributor.authorPick M.
dc.contributor.authorReiner M.
dc.contributor.authorSrivastava N.
dc.contributor.authorTripathi D.
dc.contributor.authorVourlidas A.
dc.contributor.authorWang Y.-M.
dc.contributor.authorZhang J.
dc.date.accessioned2024-03-13T01:42:37Z
dc.date.available2024-03-13T01:42:37Z
dc.date.issued2006
dc.description.abstractCMEs 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. © Springer Science+Business Media Inc. 2006.
dc.description.firstpage127
dc.description.issuenumber1-3
dc.description.lastpage176
dc.description.volume123
dc.identifier.doi10.1007/s11214-006-9016-y
dc.identifier.issn0038-6308
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/37796
dc.relation.ispartofSpace Science Reviews
dc.rightsAcesso Restrito
dc.subject.otherlanguageCoronal mass ejections (CMEs)
dc.subject.otherlanguageEruptive prominences
dc.subject.otherlanguageFlares
dc.subject.otherlanguageICMEs
dc.subject.otherlanguageInterplanetary shock waves
dc.subject.otherlanguageMagnetic reconnection
dc.subject.otherlanguageRadio bursts
dc.subject.otherlanguageSolar corona
dc.subject.otherlanguageSolar energetic particles (SEPs)
dc.subject.otherlanguageSolar magnetic field
dc.subject.otherlanguageSolar wind
dc.subject.otherlanguageSpace weather
dc.titleCoronal observations of CMEs : Report of working group A
dc.typeArtigo
local.scopus.citations69
local.scopus.eid2-s2.0-33751528806
local.scopus.subjectCoronal mass ejections (CME)
local.scopus.subjectInterplanetary Coronal mass ejections (ICME)
local.scopus.subjectRadio bursts
local.scopus.subjectSolar corona
local.scopus.subjectSolar Energetic Particles (SEP)
local.scopus.subjectSolar wind
local.scopus.updated2024-05-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=33751528806&origin=inward
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