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Solar coronal heati...
Solar coronal heating by plasma waves
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- Bingham, Robert (författare)
- Rutherford Appleton Laboratory, Chilton, Oxon, OX11 0QX, UK
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Shukla, Padma Kant (författare)
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- Eliasson, Bengt (författare)
- Umeå universitet,Institutionen för fysik
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- Stenflo, Lennart (författare)
- Umeå universitet,Institutionen för fysik
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(creator_code:org_t)
- Cambridge university, 2010
- 2010
- Engelska.
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Ingår i: Journal of Plasma Physics. - : Cambridge university. - 0022-3778 .- 1469-7807. ; 76:2, s. 135-158
- Relaterad länk:
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https://urn.kb.se/re...
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https://doi.org/10.1...
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Abstract
Ämnesord
Stäng
- The solar coronal plasma is maintained at temperatures of millions of degrees, much hotter than the photosphere, which is at a temperature of just 6000 K. In this paper, the plasma particle heating based on the kinetic theory of wave–particle interactions involving kinetic Alfvén waves and lower-hybrid drift modes is presented. The solar coronal plasma is collisionless and therefore the heating must rely on turbulent wave heating models, such as lower-hybrid drift models at reconnection sites or the kinetic Alfvén waves. These turbulent wave modes are created by a variety of instabilities driven from below. The transition region at altitudes of about 2000 km is an important boundary chromosphere, since it separates the collision-dominated photosphere/chromosphere and the collisionless corona. The collisionless plasma of the corona is ideal for supporting kinetic wave–plasma interactions. Wave–particle interactions lead to anisotropic non-Maxwellian plasma distribution functions, which may be investigated by using spectral analysis procedures being developed at the present time.
Nyckelord
- fysik
- Physics
Publikations- och innehållstyp
- ref (ämneskategori)
- art (ämneskategori)
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