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dc.date.accessioned 2022-06-13T15:25:44Z
dc.date.available 2022-06-13T15:25:44Z
dc.date.issued 1987
dc.identifier.uri http://sedici.unlp.edu.ar/handle/10915/137748
dc.description.abstract The observations made during the last years have shown that the solar corona is a very inhomogeneus medium composed by a wide variety of magnetic loops. Moreover, the magnetic field plays a very important role in the energy balance of the region. We suggest that the stationary heating of the solar corona is produced by dissipation of magnetohydrodinamic turbulence. We derive an estimation of the coronal heating rate which is comparable to the rates of conductive and radiative cooling. en
dc.language es es
dc.subject Galaxias es
dc.title Calculation of the coronal heating rate by dissipation of magnetic energy en
dc.type Articulo es
sedici.identifier.issn 1669-9521 es
sedici.creator.person Gómez, D. es
sedici.creator.person Ferro Fontán, C. es
sedici.subject.materias Astronomía es
sedici.description.fulltext true es
mods.originInfo.place Asociación Argentina de Astronomía es
sedici.subtype Comunicacion es
sedici.rights.license Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)
sedici.rights.uri http://creativecommons.org/licenses/by-nc-sa/4.0/
sedici.relation.journalTitle Boletín de la Asociación Argentina de Astronomía es
sedici.relation.journalVolumeAndIssue no. 33 es
dc.rights.uri http://creativecommons.org/licenses/by-nc-sa/4.0/ es
dc.rights.license Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) es


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Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) Excepto donde se diga explícitamente, este item se publica bajo la siguiente licencia Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)