The photospheric network |
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| Authors: | G A Chapman N R Sheeley Jr |
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| Institution: | 1. Steward Observatory, University of Arizona, Kitt Peak National Observatory, Tucson, Ariz., U.S.A.
2. Kitt Peak National Observatory, Tucson, Ariz., U.S.A.
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| Abstract: | Spectroheliograms, obtained in certain Fraunhofer lines with the 82-cm solar image at the Kitt Peak National Observatory, show a bright photospheric network having the following properties: - It resembles, but does not coincide with, the chromospheric network, the structure of the photospheric network being finer and more delicate than the relatively coarse structure of the chromospheric network.
- It is exactly cospatial with the network of non-sunspot photospheric magnetic fields.
- Its visibility in a given photospheric Fraunhofer line is primarily dependent on the states of ionization and excitation from which the line is formed and secondarily dependent on the Zeemansensitivity of the line-being most visible in low-excitation lines of neutral atoms and least visible in high-excitation lines of singly ionized atoms.
We conclude that these magnetic regions of the solar atmosphere are a few hundred degrees hotter than their surroundings, and that they are visible in white light near the limb as photospheric faculae. |
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