The Structure of the Quiet Photosphere and the Low Chromosphere
The Structure of the Quiet Photosphere and the Low Chromosphere pp 26-27 | Cite as
Spectrum Measurements of the Sun near 1 cm Wavelength
David H. Staelin
Norman E. Gaut
Sara E. Law
Woodruff T. SullivanIII
The solar brightness temperature was measured at frequencies of 19.0, 21.0, 22.2, 23.5, and 25.5 GHz on 8 days in February and March, 1966. The observed average brightness temperatures were 10 800, 10 900, 11 000, 10 700, and 9 800°K, respectively. The daily values were close to these averages.
Brightness Temperature Spectrum Measurement Antenna Pattern Lincoln Laboratory Reidel Publishing Company
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
Moran, J. M.: 1965, Radiometric Observations of the Moon near One-Centimeter Wavelength. S. M. Thesis, Department of Electrical Engineering, Massachusetts Institute of Technology, Cambridge, Mass.Google Scholar
Staelin, D. H., and Barrett, A. H.: 1966, 'Spectral Measurements of Venus Near 1-Centimeter Wavelength', Astrophys. J. 144, 352–363.ADSCrossRefGoogle Scholar
© D. Reidel Publishing Company, Dordrecht, Holland 1968
1.Research Laboratory of ElectronicsM.I.TCambridgeUSA
2.University of MarylandUSA
About this paper
Cite this paper as:
Staelin D.H., Gaut N.E., Law S.E., Sullivan W.T. (1968) Spectrum Measurements of the Sun near 1 cm Wavelength. In: de Jager C. (eds) The Structure of the Quiet Photosphere and the Low Chromosphere. Springer, Dordrecht
DOI https://doi.org/10.1007/978-94-010-3470-8_2
Publisher Name Springer, Dordrecht
Print ISBN 978-94-010-3472-2
Online ISBN 978-94-010-3470-8
Cite paper
Buy paper (PDF)