Hostname: page-component-7479d7b7d-rvbq7 Total loading time: 0 Render date: 2024-07-13T22:23:24.187Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolutionary Relation between Type I Storm Activity and the S-Component at Centimetre Wavelengths

Published online by Cambridge University Press:  25 April 2016

K. Kai  and
H. Sekiguchi
K. Kai*
Affiliation:
Tokyo Astronomical Observatory, University of Tokyo
H. Sekiguchi
Affiliation:
Tokyo Astronomical Observatory, University of Tokyo
*
* Present address: Division of Radiophysics, CSIRO, Sydney, Australia.
Get access Rights & Permissions [Opens in a new window]

Extract

Type I storms are the most frequently observed solar phenomena at metre and decimetre wavelengths. Since the first identification of the emission of this type with a large sunspot group a great many type I storms have been recorded with radio-spectrographs, polarimeters and interferometers (see, for example, Wild, Smerd and Weiss, Kundu, Wild). Nevertheless, we can offer no satisfactory answers to the most fundamental questions about type I storms: ‘What kind of disturbances supply energy to a localized coronal region to maintain the storm activity for up to several days?’; ‘What is the emission mechanism responsible for the peculiar features observed in type I storms?’.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 4 , October 1973 , pp. 217 - 219
Copyright
Copyright © Astronomical Society of Australia 1973

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

1 McCready, L.L., Pawsy, J.L., and Payne-Scott, , Ruby, , Proc. Roy. Soc. A., 190, 357 (1947).Google Scholar
2 Wild, J.P., Smerd, S.F., and Weiss, A., Ann. Rev. Astr. Astrophys., 1, 291 (1963).Google Scholar
Kundu, M.R., ‘ Solar Radio Astronomy ’, Interscience Publishers, New York (1965).Google Scholar
4 Wild, J.P., Proc. Astr. Soc. Aust. 1, 365 (1970).Google Scholar
Dodson, H.W., Hedeman, E.R. and Owren, L., Astrophys. J., 118, 169 (1953).Google Scholar
6 Dodson, H.W., Proc. Instn. Radio Engrs., 46, 149 (1958).Google Scholar
7 Mallinge, A.M., Ann. Astrophys., 23, 574 (1960).Google Scholar
8 Takakura, T., Tsuchiya, A., Morimoto, M., and Kai, K., Proc. Astr. Soc. Aust., 1, 56 (1967).Google Scholar
9 Tanaka, H., Kakinuma, T., and Énomé, S., Proc. Res. Inst. Atmos. Nagoya Univ., 14, 23 (1967).Google Scholar
10 Tanaka, H., Kakinuma, T., Énomé, S., Torii, G., Tsukiji, Y., and Kobayashi, S., Proc. Res. Inst. Atmos. Nagoya Univ., 16, 113 (1969).Google Scholar
11 Solar-Geophysical Data: U.S. Dept. of Commerce, National Oceanic and Atmospheric Administration Environmental Data Service (1970–1972).Google Scholar
12 Tanaka, H., and Kakinuma, T., Rep. lonos. Space Res. Japan, 18, 32 (1964).Google Scholar
13 Kakinuma, T., and Swarup, G., Astrophys. J., 136, 975 (1962).Google Scholar