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Evidence on Chromospheric Structure from Observations of Solar Brightness Distribution at Millimetre Wavelengths

Published online by Cambridge University Press:  25 April 2016

N. R. Labrum
N. R. Labrum*
Affiliation:
Division of Radiophysics, CSIRO, Sydney
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Extract

Observations of the distribution of millimetre-wavelength brightness over the quiet Sun provide an important test of models of the solar chromosphere. The author and colleagues have recently carried out two investigations of the quiet-Sun brightness at 3 mm wavelength — one by means of a total eclipse observation (Labrum et al. 1978) and the other by aperture synthesis with a two-element interferometer (Archer et al. 1978). I present here a preliminary discussion of these and other measurements of millimetre-wavelength brightness distributions and of their interpretation in terms of chromospheric structure.

Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 3 , Issue 4 , 1978 , pp. 256 - 259
Copyright
Copyright © Astronomical Society of Australia 1978

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References

Ade, P. A. R., Rather, J. D. G., and Clegg, P. E., Astrophys. J., 187, 389 (1974).CrossRefGoogle Scholar
Archer, J. W., Ph.D. Thesis, University of Sydney (1977).Google Scholar
Archer, J. W., Labrum, N. R., and Scarpellino, C. J., ‘Measurement of the solar brightness distribution at X = 3 mm by an aperture synthesis method’ (in preparation) (1978).Google Scholar
Beckers, J.M., Solar Phys., 3, 367 (1968).Google Scholar
Beckers, J. M., Ann. Rev. Astron. Astrophys., 10, 73 (1972).Google Scholar
Beckman, J. E., Clark, C. D., and Ross, J., Solar Phys., 31, 319 (1973).Google Scholar
Coates, R. J., Gibson, J. E., and Hagen, J. P., Astrophys. J., 128, 406 (1958).Google Scholar
Gabriel, A. H., Phil. Trans. R. Soc. Lond., A281, 339 (1976).Google Scholar
Hiei, E., Pubi. Astron. Soc. Japan, 15, 277 (1963).Google Scholar
Kawabata, K.-A., and Sofue, Y., Pubi. Astron. Soc. Japan, 24, 469 (1972).Google Scholar
Kislyakov, A. G., Kuznetsov, I. V., Kuznetsova, N. A., Chernyshev, V. I., and Serov, N. V.,Astron. Zh., 51, 1036 (1974) (English trans. Sov. Astron., 181, 612 (1975)).Google Scholar
Kundu, M. R., and Liu, S.-Y., Solar Phys., 44, 361 (1975).CrossRefGoogle Scholar
Labrum, N. R., Archer, J. W., and Smith, C. J., ‘The solar brightness distribution at 3 mm wavelength from observations of the eclipse of 1976 October 23’, Solar Phys. (in press, 1978).CrossRefGoogle Scholar
Lantos, P., and Kundu, M. R., Astron. Astrophys., 21, 119 (1972).Google Scholar
Shimabukuro, F. I., Wilson, W. J., Mori, J. T., and Smith, P. L., Solar Phys., 40, 359 (1975).Google Scholar
Simon, M., and Zirin, H., Solar Phys., 9, 317 (1969).Google Scholar
Suzuki, I., Kawabata, K.-A., and Ogawa, H., Solar Phys., 46, 205 (1976).Google Scholar
Swanson, P. N., and Hagen, J. P., Solar Phys., 43, 57 (1975).Google Scholar
Vernazza, J. E., AND Noyes, R. W., Solar Phys., 22, 358 (1972).CrossRefGoogle Scholar
Vernazza, J. E., Averett, E. H., and Loeser, R., Astrophys. J., 184, 605 (1973).Google Scholar