Abstract
The filamentary structure of the magnetic fields as well as the coherent radiations that emanate from a sunspot are explained considering solar burst as a non-equilibrium process. Methods of irreversible statistical mechanics have been applied to the problem of an electron gas in a constant magnetic field to explain the above features. We have obtained the non-equilibrium distribution function in the self-consistent field approximation. The dielectric function, we obtained, is a function of time, besides being a function of frequency and wavevector. We have thus taken the non-linearity of the system as well. This theory explains many features of stria bursts, chain bursts as well as the type III bursts. This also accounts for the bunching of the magnetic field lines as a consequence of quantisation of flux in the Landau sense.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Coppi B and Frieland A B 1971Astrophys. J. 1169 379
De Jager C 1968Proc. Symp. Solar Flares and Space Research (North Holland, Amsterdom) p. 1
de la Nöe J and Boischot A 1972Astron. Astrophys. 20 55
Friedman M and Hamberger S M 1969Solar Phys. 8 104
Landau L D and Lifshitz E M (1959)Statistical physics (Pergamon Press, London)
Moreton G E and Severny A B 1968Solar Phys. 3 282
Pratap R 1967Il Nuovo Cimento 52 B 63
Pratap R, Vasudevan R and Sridhar R 1972a Il Nuovo Cimento 8 B 223
Pratap R and Sridhar R 1972b Il Nuovo Cimento 9 B 279
Pratap R 1974a Il Nuovo Cimento 19 B 29
Pratap R 1974b Il Nuovo Cimento 19 B 44
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Pratap, R. The filamentary structure of the sunspot magnetic fields. Pramana - J. Phys 2, 327–335 (1974). https://doi.org/10.1007/BF02847246
Received:
Issue Date:
DOI: https://doi.org/10.1007/BF02847246