Abstract
The data from a high counting rate neutron monitor has been analysed to study the nature of galactic cosmic-ray transient modulation associated with three classes of magnetic clouds, i.e., clouds associated with shock, stream interface and cold magnetic enhancement.
It is found that the decreases in cosmic-ray intensity which are associated with clouds preceded by a shock, are very high (Forbush-type) and these decreases start earlier than the arrival of the cloud at the Earth. From the study of the time profile of these decreases it is found that the onset time of a Forbush-type decrease produced by a shock-associated cloud starts nearly at the time of arrival of the shock front at the Earth and the recovery is almost complete within a week.
The decreases in cosmic-ray intensity associated with clouds followed by a stream interface are smaller in magnitude and larger in duration. The depression starts on the day of the arrival of the cloud.
The decreases associated with the third category of clouds, i.e., clouds associated with cold magnetic enhancement (a region in which plasma temperature is anomalously low and the magnetic field strength is enhanced) are of still smaller amplitude and duration. The decrease in this case starts on the day the cloud arrives at the Earth.
It seems that the Forbush decrease modulating region consists of a shock front followed by a plasma sheath in which the field intensity is high and turbulent. The amplitude of decrease is related to the field magnitude and the speed of the cloud. Both shocked plasma and the magnetic cloud are influential in determining the time profile of these decreases. In our view it is not the magnetic field strength or the topology alone which is responsible for the cosmic-ray depression. The most likely additional effect is the increased degree of turbulence.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Ankiewicz, P. J., Stoker, P. H., and Moraal, H.: 1983, Proc. 18th Int. Cosmic Ray Conf. 10, 120.
Barnden, L. R.: 1973, Proc. 13th Int. Cosmic Ray Conf. 2, 1277.
Barouch, E. and Burlaga, L. F.: 1975, J. Geophys. Res. 80, 449.
Barouch, E. and Sari, J. W.: 1976, J. Geophys. Res. 81, 1453.
Borrini, G., Gosling, J. T., Bame, S. J., and Feldman, W. C.: 1982, J. Geophys. Res. 87, 4365.
Burlaga, L. F.: 1983, Proc. 18th Int. Cosmic Ray Conf. 12, 21.
Burlaga, L. F. and Behannon, K. W.: 1982, Solar Phys. 81, 181.
Burlaga, L. F. and King, J. H.: 1979, J. Geophys. Res. 84, 6633.
Burlaga, L. F. and Klein, L. W.: 1980, NASA Techn. Mem. 80668.
Burlaga, L. F., Klein, L. W., Sheeley, Jr., N. R., Michels, D. J., Howard, R. A., Kooman, M. J., Schwenn, R., and Rosenbaur, H.: 1982, Geophys. Res. Letters 9, 1317.
Burlaga, L. F., McDonald, F. B., Ness, N. F., Schwenn, R., Lazarus, A. J., and Mariani, F.: 1984, J. Geophys. Res. 89, 6579.
Burlaga, L. F. and Oglvie, K. W.: 1969, J. Geophys. Res. 74, 2815.
Burlaga, L. F., Sittler, E., Mariani, F., and Schwenn, R.: 1981, J. Geophys. Res. 86, 6673.
Duggal, S. P., Pomerantz, M. A., Schaefer, R. K., and Tsao, C. H.: 1983, J. Geophys. Res. 88, 2973.
Forbush, S. E.: 1938, Phys. Rev. 54, 975.
Fujimoto, K., Kojima, H., and Murakami, K.: 1983, Proc. 18th Int. Cosmic Ray Conf. 3, 267.
Geranios, A.: 1982, Astrophys. Space Sci. 81, 103.
Geranios, A. and Rosenbauer, H.: 1983, Proc. 18th Int. Cosmic Ray Conf. 4, 206.
Gold, T.: 1959, J. Geophys. Res. 64, 1665.
Goldstein, M. L., Burlaga, L. F., and Matthaeus, W. H.: 1984, J. Geophys. Res. 89, 3747.
Hundhausen, A. J., Sawyer, C. B., House, L., Illings, R. M. E., and Wagner, W. J.: 1984, J. Geophys. Res. 89, 2639.
Iucci, N., Parisi, M., Storini, M., and Villoresi, G.: 1979a, Nuovo Cimento 2C, 1.
Iucci, N., Parisi, M., Storini, M., and Villoresi, G.: 1979b, Nuovo Cimento 2C, 421.
Kane, R. P.: 1977, J. Geophys. Res. 82, 561.
Klein, L. W. and Burlaga, L. F.: 1982, J. Geophys. Res. 87, 613.
Laster, H., Lenchek, A. M., and Singer, S. F.: 1962, J. Geophys. Res. 67, 2639.
Lockwood, J. A.: 1971, Space Sci. Rev. 12, 658.
Lockwood, J. A., Hsieh, L. and Quenby, J. J.: 1975, J. Geophys. Res. 80, 1725.
Lockwood, J. A. and Webber, W. R.: 1977, J. Geophys. Res. 82, 1906.
Lockwood, J. A. and Webber, W. R.: 1984, J. Geophys. Res. 89, 17.
McDonald, F. B., Trainor, J. H., and Webber, W. R.: 1981, Proc. 17th Int. Cosmic Ray Conf. 10, 147.
Morfill, G., Richter, A. K., and Scholer, M.: 1979, J. Geophys. Res. 84, 1505.
Morrison, P.: 1954, Phys. Rev. 95, 641.
Morrison, P.: 1956, Phys. Rev. 101, 1354.
Murayama, T., Maezawa, K., and Hakamada, K.: 1979, Proc. 16th Int. Cosmic Ray Conf. 3, 416.
Newkirk, G. Jr., Hundhausen, A. J., and Pizzo, V.: 1981, J. Geophys. Res. 86, 5387.
Nishida, A.: 1982, J. Geophys. Res. 87, 6003.
Palmer, I. D., Allum, F. R., and Singer, S.: 1978, J. Geophys. Res. 83, 75.
Parker, E. N.: 1963, in Interplanetary Dynamical Processes, Interscience, New York.
Piddington, J. H.: 1958, Phys. Rev. 112, 589.
Quenby, J. J.: 1971, Proc. 12th Int. Cosmic Ray Conf. 2, 730.
Sanderson, T. R., Marsden, R. G., Reinhard, R., Wenzel, K. P., and Smith, E. J.: 1983, Geophys. Res. Letters 10, 916.
Stoker, P. H. and Carmichael, H.: 1971, Astrophys. J. 169, 357.
Thomas, B. T. and Gall, R.: 1984, J. Geophys. Res. 89, 2991.
Van Allen, J. A.: 1979, Geophys. Res. Letters 6, 566.
Venkatesan, D., Shukla, A. K., and Agrawal, S. P.: 1982, Solar Phys. 81, 375.
Wagner, W. J.: 1984, Ann. Rev. Astron. Astrophys. 22, 267.
Wilson, R. M. and Hildner, E.: 1984, Solar Phys. 91, 169.
Zirker, J. B. (ed.): 1977, Coronal Holes and High Speed Streams; A monograph from Skylab Workshop I, Colorado Associated University Press, Boulder, Colo., U.S.A.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Badruddin, Yadav, R.S. & Yadav, N.R. Influence of magnetic clouds on cosmic ray intensity variation. Sol Phys 105, 413–428 (1986). https://doi.org/10.1007/BF00172057
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00172057