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On the predominance of the radial component of the magnetic field in the solar corona

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dc.contributor.author Habbal, S. R. en_US
dc.contributor.author Woo, R. en_US
dc.contributor.author Arnaud, J. en_US
dc.date.accessioned 2004-09-17T06:45:58Z
dc.date.available 2004-09-17T06:45:58Z
dc.date.issued 2002
dc.identifier.citation Astrophysical journal en_US
dc.identifier.clearanceno 02-1622
dc.identifier.uri http://hdl.handle.net/2014/9406
dc.description.abstract In this paper, the polarized intensity measurements of the Fe XIII 10747 A line described by Arnaud are placed, for the first time, in the context of the corresponding pB images from the HAO Mauna Loa MkIII K-Coronameter, which first became available in 1980. It is shown how the predominance of the radial direction of the coronal magnetic field at solar maximum is consistent with radially expanding magnetic field lines coexisting with the large-scale structures associated with streamers. en_US
dc.format.extent 3101261 bytes
dc.format.mimetype application/pdf
dc.language.iso en_US
dc.subject.other solar wind corona en_US
dc.title On the predominance of the radial component of the magnetic field in the solar corona en_US


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