The effects of Alfvén waves on heating plasma in post-flare loops
- 36 Downloads
- 1 Citations
Abstract
In investigating the effects of collision Alfvén waves on the heating of a cool-type solar loop, like the post-flare loop, models are proposed, and the distributions of ion or electron density, temperature, pressure, and wave energy density are simulated. We assumed the magnetic field strength in the loop is about 100 G and found that Alfvén waves can propagate through the whole loop, that is to say, the decay length of collision Alfvén waves which we consider can reach to the height or length of the loop. Thus, the Alfvén wave heating is a considerable heating mechanism in cool loops. And we also found that the variations of density, pressure, and wave energy density are more significant than those of the temperature. In the whole loop, the temperature is of the order of ∼104 K. In comparison with other parameters, the temperature can be considered as homogeneous; hence, the heat conductive flux in the simulations is omitted.
Keywords
Magnetic Field Energy Density Field Strength Wave Energy Magnetic Field StrengthPreview
Unable to display preview. Download preview PDF.
References
- Cheng, C.-C., Oran, E.S., Doschek, G. A., Boris, J. P., and Mariska, J. T.: 1983,Astrophys. J. 265, 1090.Google Scholar
- Dewar, R. L.: 1970,Phys. Fluids 13, 2710.Google Scholar
- Fisher, G. H., Canfield, R. C., and McClymont, A. N.: 1985a,Astrophys. J. 289, 414.Google Scholar
- Fisher, G. H., Canfield, R. C., and McClymont, A. N.: 1985b,Astrophys. J. 289, 425.Google Scholar
- Fisher, G. H., Canfield, R. C., and McClymont, A. N.: 1985c,Astrophys. J. 289, 434.Google Scholar
- Jacques, S. A.: 1977,Astrophys. J. 215, 942.Google Scholar
- Kaplan, S. A. and Tsytovich, V. N.: 1973,Plasma Astrophysics, Pergamon, New York, p. 25 (since this English translation has some errors in the mathematical expressions, the original Russian publication should be consulted).Google Scholar
- Klimchuk, J. A.: 1989, (priv. comm.).Google Scholar
- Klimchuk, J. A. and Mariska, J. T.: 1988,Astrophys. J. 328, 334.Google Scholar
- Lang, K. R. et al.: 1984,Adv. Space Res. 4, 105.Google Scholar
- Li, X. Q.: 1990, (priv. comm.).Google Scholar
- Li, X. Q., Zhang, Z., and Zhang, Y.: 1984,Solar Phys. 91, 289.Google Scholar
- Lin, J., Zhang, Z., Wang, Z. and Smartt, R. N.: 1989,Acta Astron. Sinica 30, 52.Google Scholar
- Lin, J., Zhang, Z., Wang, Z., and Smartt, R. N.: 1990,Acta Astron. Sinica 31, 313.Google Scholar
- MacNeice, P.: 1986,Solar Phys. 103, 47.Google Scholar
- McClymont, A. N.: 1989, (priv. comm.).Google Scholar
- Mihalas, D.: 1978,Stellar Atmospheres, W. H. Freeman and Co., San Francisco.Google Scholar
- Moore, R. L. and Fung, P. C. W.: 1972,Solar Phys. 23, 78.Google Scholar
- Nagai, F.: 1980,Solar Phys. 68, 351.Google Scholar
- Osterbrock, D. E.: 1961,Astrophys. J. 134, 347.Google Scholar
- Pallavicini, R., Peres, G., Serio, S., Vaiana, G., Acton, L., Leibacher, J., and Rosner, R.: 1983,Astrophys. J. 270, 270.Google Scholar
- Ricchiazzi, P. J.: 1982, Ph.D. Thesis, University of California, San Diego.Google Scholar
- Somov, B. V., Sermulina, B. J. and Spekter, A. R.: 1981,Solar Phys. 81, 281.Google Scholar
- Švestka, Z.: 1976,Solar Flares, D. Reidel Publ. Co., Dordrecht, Holland, p. 311.Google Scholar
- Tajima, T., Brunel, F., and Sakai, J.: 1982,Astrophys. J. 258, L45.Google Scholar
- Uchida, Y. and Kaburaki, O.: 1974,Solar Phys. 35, 451.Google Scholar
- Wentzel, D. G.: 1974,Solar Phys. 39, 129.Google Scholar
- Zhang, Z., Lin, J., and Wang, Z.: 1989,Acta Astrophys. Sinica 9, 68.Google Scholar