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dc.contributor.authorVranjes, J.
dc.date2011
dc.date.accessioned2016-03-29T12:43:54Z
dc.date.available2016-03-29T12:43:54Z
dc.identifier.urihttps://orfeo.belnet.be/handle/internal/3150
dc.descriptionThe EIT waves named after the extreme-ultraviolet imaging telescope (EIT) onboard the solar and heliospheric observatory (SOHO) are in the literature usually described as fast magneto-acoustic (FMA) modes. However, observations show that a large percentage of these events propagate with very slow speeds that may be as low as 20 km/s. This is far below the FMA wave speed which cannot be below the sound speed, the latter being typically larger than 10 2 km/s in the corona. In the present study, it is shown that, to account for such low propagation speed, a different wave model should be used, based on the theory of gravity waves, both internal (IG) and surface (SG) ones. The gravity modes are physically completely different from the FMA mode, as they are essentially dispersive and in addition the IG wave is a transverse mode. Both the IG and the SG mode separately can provide proper propagation velocities in the whole low speed range.
dc.languageeng
dc.titleSlow EIT waves as gravity modes
dc.typeArticle
dc.subject.frascatiPhysical sciences
dc.audienceScientific
dc.subject.freeExtreme-ultraviolet imaging telescopes
dc.subject.freeGravity modes
dc.subject.freeLow speed
dc.subject.freeLow-propagation
dc.subject.freePropagation velocities
dc.subject.freeSolar and heliospheric observatories
dc.subject.freeSound speed
dc.subject.freeTheory of gravity
dc.subject.freeTransverse mode
dc.subject.freeWave models
dc.subject.freeWave speed
dc.subject.freeMagnetoacoustic effects
dc.subject.freeSpeed
dc.subject.freeDiagnostic radiography
dc.source.titlePhysics of Plasmas
dc.source.volume18
dc.source.issue6
dc.source.page62902
Orfeo.peerreviewedYes
dc.identifier.doi10.1063/1.3597136
dc.identifier.scopus2-s2.0-79960170031


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