Hale, George E. and Ellerman, Ferdinand (1916) The Minute Structure of the Solar Atmosphere. Proceedings of the National Academy of Sciences of the United States of America, 2 (2). pp. 102-109. ISSN 0027-8424. http://resolver.caltech.edu/CaltechAUTHORS:HALpnas16b
- Published Version
See Usage Policy.
Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:HALpnas16b
During a total eclipse of the sun, when the light of the disk is completely cut off by the moon, the solar atmosphere is momentarily revealed. The exceedingly faint corona, extending millions of miles into space, can be seen only at such times. But the more brilliant chromosphere, the comparatively shallow atmosphere of luminous gases which completely encircles the sun, and the prominences which rise out of it, can be observed on any clear day with the aid of a spectroscope. First applied to this purpose in 1868, the spectroscope has yielded a large store of information regarding the number, distribution, and nature of the prominences and the structure of the upper chromosphere, as seen in elevation at the sun's limb. It has also permitted the observation of certain phenomena of the solar atmosphere in projection against the disk, but on account of the brilliant background, only their general outlines can be thus detected. In order to study their details, we must have recourse to the spectroheliograph.
|Additional Information:||Copyright © 1916 by the National Academy of Sciences. Received by the Academy, January 10, 1916.|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Archive Administrator|
|Deposited On:||20 Sep 2008 03:57|
|Last Modified:||14 Nov 2014 19:20|
Repository Staff Only: item control page