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High-resolution images of a solar coronal hole obtained by SOHO’s SUMER instrument on 28 and 29 July 1996. These observations in four spectral lines are representative of different temperature regimes in the solar atmosphere. The emission lines from top to bottom are:- Fe XII with a wavelength of 12...
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ftciteseerx:oai:CiteSeerX.psu:10.1.1.230.8624 2023-05-15T18:22:29+02:00 Printed in Uri Feldman Ingolf E. Dammasch Klaus Wilhelm Donald M. Hassler Bruce Battrick The Pennsylvania State University CiteSeerX Archives 2003 application/pdf http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.230.8624 http://ads.harvard.edu/books/2003isua.book/SUMERfirstpages.pdf en eng http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.230.8624 http://ads.harvard.edu/books/2003isua.book/SUMERfirstpages.pdf Metadata may be used without restrictions as long as the oai identifier remains attached to it. http://ads.harvard.edu/books/2003isua.book/SUMERfirstpages.pdf Editor Layout text 2003 ftciteseerx 2016-01-07T18:44:21Z High-resolution images of a solar coronal hole obtained by SOHO’s SUMER instrument on 28 and 29 July 1996. These observations in four spectral lines are representative of different temperature regimes in the solar atmosphere. The emission lines from top to bottom are:- Fe XII with a wavelength of 1241.990 Å and a formation temperature of 1.4 x 10 6 K- Mg X with a wavelength of 624.965 Å and a formation temperature of 1.1 x 10 6 K- N V with a wavelength of 1238.821 Å and a formation temperature of 1.9 x 10 5 K, and- C I with a wavelength of 1249.405 Å and a formation temperature of just over 1.3 x 10 4 K. The C I image shows the chromospheric network. Spicules and a pronounced limb brightening can be seen in N V. The Mg X exposure highlights the polar plumes and coronal bright points, whereas the Fe XII image outlines the coronal hole and its boundaries. (The displays of the solar south pole are inverted for graphical reasons.) Published by Text South pole Unknown South Pole |
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Editor Layout Uri Feldman Ingolf E. Dammasch Klaus Wilhelm Donald M. Hassler Bruce Battrick Printed in |
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High-resolution images of a solar coronal hole obtained by SOHO’s SUMER instrument on 28 and 29 July 1996. These observations in four spectral lines are representative of different temperature regimes in the solar atmosphere. The emission lines from top to bottom are:- Fe XII with a wavelength of 1241.990 Å and a formation temperature of 1.4 x 10 6 K- Mg X with a wavelength of 624.965 Å and a formation temperature of 1.1 x 10 6 K- N V with a wavelength of 1238.821 Å and a formation temperature of 1.9 x 10 5 K, and- C I with a wavelength of 1249.405 Å and a formation temperature of just over 1.3 x 10 4 K. The C I image shows the chromospheric network. Spicules and a pronounced limb brightening can be seen in N V. The Mg X exposure highlights the polar plumes and coronal bright points, whereas the Fe XII image outlines the coronal hole and its boundaries. (The displays of the solar south pole are inverted for graphical reasons.) Published by |
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The Pennsylvania State University CiteSeerX Archives |
format |
Text |
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Uri Feldman Ingolf E. Dammasch Klaus Wilhelm Donald M. Hassler Bruce Battrick |
author_facet |
Uri Feldman Ingolf E. Dammasch Klaus Wilhelm Donald M. Hassler Bruce Battrick |
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Uri Feldman |
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2003 |
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http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.230.8624 http://ads.harvard.edu/books/2003isua.book/SUMERfirstpages.pdf |
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http://ads.harvard.edu/books/2003isua.book/SUMERfirstpages.pdf |
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http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.230.8624 http://ads.harvard.edu/books/2003isua.book/SUMERfirstpages.pdf |
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Metadata may be used without restrictions as long as the oai identifier remains attached to it. |
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