The coarse structure of the solar atmosphere
Abstract
Observations of the quiet sun at wavelengths from 3 Å to 75 cm show (with two exceptions: the Ovi line at 1032 Å and possibly the continuum at 1.2 mm) either no limb brightening or less than had been supposed. On the other hand, the brightness temperature is observed to increase with wavelength in the millimeter and centimeter range. If this increase is due to greater visibility of hot overlying material, that material ought to be evident at the limb at shorter wavelengths, resulting in limb brightening. The only possible explanation for the absence of limb brightening at almost all wavelengths is that the emitting surface is rough at all wavelengths, with a scale of roughness approximately equal to the scale height at each temperature. Contradictions with existing models, along with the additional observations required for an improved model are discussed.
Additional Information
© 1969 Kluwer Academic Publishers. Provided by the NASA Astrophysics Data System. Received 19 May 1969; Issue Date October 1969. This research was supported by the National Science Foundation under GP-7030 and the National Aeronautics and Space Administration under grant NGR 05 002 034. We are very grateful to A. Tlamicha for sending to us the 2 cm data in advance of publication, and to A.T. Moffet for obtaining the 3 cm data at Goldstone. We thank K. Chu for assistance with some of the model calculations.Attached Files
Published - 1969SoPh____9__317S.pdf
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Additional details
- Eprint ID
- 104178
- Resolver ID
- CaltechAUTHORS:20200701-074915411
- GP-7030
- NSF
- NGR 05 002 034
- NASA
- Created
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2020-07-01Created from EPrint's datestamp field
- Updated
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2021-11-16Created from EPrint's last_modified field