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Magnetic nature of coronal loops

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dc.contributor.author Singh, J
dc.contributor.author Muneer, S
dc.contributor.author Sakurai, T
dc.contributor.author Ichimoto, K
dc.date.accessioned 2009-08-06T10:27:51Z
dc.date.available 2009-08-06T10:27:51Z
dc.date.issued 2007-12
dc.identifier.citation Bulletin of the Astronomical Society of India, Vol. 35, No. 4, pp. 437 - 445 en
dc.identifier.issn 0304-9523
dc.identifier.uri http://hdl.handle.net/2248/4723
dc.description.abstract It is generally believed that the magnetic pressure is much higher than the gas pressure in the coronal loops and these loops are isothermal in nature. We made systematic observations of four strong coronal emission lines in the visible and near infrared part of the spectrum for about 8 years. Two emission lines were observed at a time, making raster scans of a steady coronal region. We studied the variation of line widths of these lines and intensity ratios as a function of height. The relationship between the widths of these lines and intensity ratios indicates that the steady coronal loops are not magnetically isolated. These findings put restrictions on coronal loop models and indicate that the magnetic pressure in coronal loops may be much less than assumed. These results strongly suggest that magnetic field strength in the corona needs to be measured accurately. en
dc.language.iso en en
dc.publisher Astronomical Society of India en
dc.relation.uri http://www.ncra.tifr.res.in/~basi/07December/Abstracts/354372007.htm en
dc.rights © Astronomical Society of India en
dc.subject Solar Corona en
dc.subject Coronal Loops en
dc.subject Emission Lines en
dc.subject Spectroscopy en
dc.subject Line Width en
dc.subject Intensity Ratio en
dc.title Magnetic nature of coronal loops en
dc.type Article en

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