Abstract
We suggest that the solar corona is stationarily heated by Joule dissipation of magnetohydrodynamic (MHD) turbulence. This turbulence is continuously being fed by subphotospheric convective motions at very low wavenumbers where the plasma can be considered ideal. The cascade process due to the nonlinear interaction of the turbulent modes, effectively transfers energy to even shorter wavenumbers until Joule effect becomes dominant and converts the cascading magnetic energy into heat.
Assuming that a stationary spectrum is established, we show that MHD turbulence naturally provides a way of enhancing the Joule dissipation of macroscopic magnetic stresses and a heating rate can be derived.
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References
Antiochos, S. K.: 1987, Astrophys. J. 312, 886.
Bornmann, P.: 1987, Astrophys. J. 313, 449.
Braginskii, S. I.: 1985, Rev. Plasma Phys. 1, 205.
Browning, P. K., Sakurai, T., and Priest, E. R.: 1986, Astron. Astrophys. 158, 217.
Dobrowolny, M., Mangeney, A., and Veltri, P.: 1980, Phys. Rev. Letters 45, 144.
Dowdy, J. F., Rabin, D., and Moore, R. L.: 1985, Solar Phys. 99, 35.
Fyfe, D., and Montgomery, D.: 1976, J. Plasma Phys. 16, 181.
Grappin, R.: 1986, Phys. Fluids 29, 2433.
Grappin, R., Frisch, U., Leorat, J., and Pouquet, A.: 1982, Astron. Astrophys. 105, 6.
Gratton, F., Heyn, M., Biernat, H., Rijnbeek, R., and Gnavi, G.: 1987, in 21th ESLAB Symp., Bolkeskjø, Norway, ESA (in press).
Hasegawa, A.: 1985, Adv. Phys. 34, 1.
Heyvaerts, J.: 1985, in M. Kundu and G. Holman (eds.), ‘Unstable Current Systems’, IAU Symp. 107, 95.
Heyvaerts, J. and Priest, E. R.: 1984, Astron. Astrophys. 137, 63.
Hollweg, J.: 1983, in M. Neugebauer (ed.), Solar Wind V, NASA Conf. Publ. 2280, p. 5.
Hollweg, J.: 1986a, Astrophys. J. 306, 730.
Hollweg, J.: 1986b, J. Geophys. Res. 91, 4111.
Hossain, M., Matthaeus, W. H., and Montgomery, D.: 1983, J. Plasma Phys. 30, 479.
Kraichnan, R. H. and Montgomery, D.: 1980, Rep. Progr. Phys. 43, 547.
Kuperus, M., Ionson, J. A., and Spicer, D. A.: 1981, Ann. Rev. Astron. Astrophys. 19, 7.
Martens, P: 1986, in A. I. Poland (ed.), Coronal and Prominence Plasmas, NASA Conf. Publ. 2442, p. 407.
Matthaeus, W. H. and Goldstein, M. L.: 1982, J. Geophys. Res. 87, 6011.
Matthaeus, W. H., Goldstein, M. L., and Montgomery, D.: 1983, Phys. Rev. Letters 51, 1484.
Parker, E. N.: 1972, Astrophys. J. 174, 499.
Parker, E. N.: 1981a, Astrophys. J. 244, 631.
Parker, E. N.: 1981b, , Astrophys. J. 244, 644.
Parker, E. N: 1983a, Astrophys. J. 264, 635.
Parker, E. N.: 1983b, Astrophys. J. 264, 642.
Sakurai, T. and Levine, R. H.: 1981, Astrophys. J. 248, 817.
Seehafer, N.: 1986, Solar Phys. 107, 73.
Sturrock, P. A., and Uchida, Y.: 1981, Astrophys. J. 246, 331.
Taylor, J. B.: 1974, Phys. Rev. Letters 33, 1139.
Ting, A. C., Matthaeus, W. H., and Montgomery, D.: 1986, Phys. Fluids 29, 3261.
Vaiana, G. S. and Rosner, R.: 1978, Ann. Rev. Astron. Astrophys. 16, 393.
van Ballegooijen, A. A.: 1985, Astrophys. J. 298, 421.
van Ballegooijen, A. A.: 1986, Astrophys. J. 311, 1001.
Withbroe, G. L., and Noyes, R. W.: 1977, Ann. Rev. Astron. Astrophys. 15, 363.
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Gómez, D., Fontán, C.F. Coronal heating by selective decay of MHD turbulence. Sol Phys 116, 33–44 (1988). https://doi.org/10.1007/BF00171713
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DOI: https://doi.org/10.1007/BF00171713