Abstract
One-dimensional hydrodynamic simulations are performed in order to examine the influence of initial atmospheric structures on the dynamics of spicules. This is an extended version of our previous spicule theory: spicules are produced by the shock wave (MHD slow mode shock) which originates from a bright point appearance (sudden pressure increase) at the network in the photosphere or in the low chromosphere. Simulation results well reproduce the observational facts that spicules are absent over plages and long under coronal holes. The physical reason is that the growth of a shock wave during its propagation through the chromosphere is small in plage regions and large in coronal hole regions, since the growth of a shock is determined by the density ratio (ϱ h 0/ϱ c ) between the bright point and the corona. An empirical formula ΔH max ∼ (ϱ h 0/ϱ c )0.46 is obtained, where ΔH max is the maximum height of spicules above the transition region. The cross-section of the vertical magnetic flux tube is assumed to be constant in the numerical simulations.
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Basri, G. S., Linsky, J. L., Bartoe, J. D. F., Brueckner, G., and Van Hoosier, M. E.: 1979, Astrophys. J. 230, 924.
Beckers, J. M.: 1968, Solar Phys. 3, 367.
Beckers, J. M.: 1972, Ann. Rev. Astron. Astrophys. 10, 73.
Bird, G. A.: 1964, Astrophys. J. 139, 675.
Bohlin, J. D., Vogel, S. N., Purcell, J. D., Sheeley, N. R., Jr., Tousey, R., and Van Hoosier, M. E.: 1975, Astrophys. J. 197, L133.
Bray, R. J. and Loughhead, R. E.: 1974, The Solar Chromosphere, Chapman and Hall, London.
Brinkley, S. R. Jr. and Kirkwood, J. G.: 1947, Phys. Rev. 71, 606.
Chisnell, R. E.: 1955, Proc. Roy. Soc. London A232, 350.
Frazier, E. N. and Stenflo, J. O.: 1972, Solar Phys. 27, 330.
Gabriel, A. H.: 1976, Phil. Trans. Roy. Soc. London A281, 339.
Gabriel, A. H.: 1977, in R. M. Bonnet and Ph. Delache (eds.), ‘The Energy Balance and Hydrodynamics of the Solar Chromosphere’, IAU Colloq. 36, 375.
Kogure, T. and Osaki, T.: 1962, Publ. Astron. Soc. Japan 14, 254.
Lippincott, S. L.: 1957, Smithsonian Contrib. Astrophys. 2, 15.
Nauer, D. J., Teske, R. G., and Eleste, G. E.: 1980, Solar Phys. 67, 23.
Ohno, Y., Sakashita, S., and Yamazaki, H.: 1960, Prog. Theor. Phys. 23, 294.
Ohno, Y., Sakashita, S., and Ohyama, N.: 1961, Prog. Theor. Phys. Suppl. 20, 85.
Osterbrock, D. E.: 1961, Astrophys. J. 134, 347.
Rabin, D. and Moore, R. L.: 1980, Astrophys. 241, 394.
Richtmyer, R. D. and Morton, K. W.: 1967, Difference Method for Initial Value Problem, 2nd ed., Interscience Publishers, New York.
Rubin, E. L. and Burstein, S. Z.: 1967, J. Comp. Phys. 2, 178.
Saito, M.: 1964, Publ. Astron. Soc. Japan 16, 179.
Shibata, K.: 1981, submitted to Solar Phys.
Shibata, K., Nishikawa, T., Kitai, R., and Suematsu, Y.: 1982, Solar Phys., in press (Paper II).
Stein, R. F. and Schwartz, R. A.: 1972, Astrophys. J. 177, 807.
Stenflo, J. O.: 1975, Solar Phys. 42, 79.
Stenflo, J. O.: 1976, in V. Bumba and J. Kleczek (eds.), ‘Basic Mechanism of Solar Activity’, IAU Symp. 71, 69.
Stenflo, J. O.: 1977, in R. M. Bonnet and Ph. Delache (eds.), ‘The Energy Balance and Hydrodynamics of the Solar Chromosphere and Corona’, IAU Colloq. 36, 143.
Suematsu, Y.: 1982, in preparation.
Suematsu, Y., Shibata, K., Nishikawa, T., and Kitai, R.: 1982, Solar Phys. 75, 99.
Wentzel, D. G. and Solinger, A. B.: 1967, Astrophys. J. 148, 877.
Whitham, G. B.: 1958, J. Fluid Mech. 4, 337.
Withbroe, G. L. and Noyes, R. W.: 1977, Ann. Rev. Astron. Astrophys. 15, 363.
Withbroe, G. L., Jaffe, D. T., Foukal, P. V., Huber, M. C. E., Noyes, R. W., Reeves, E. M., Schmahl, E. J., Timothy, J. G., and Vernazza, J. E.: 1976, Astrophys. J. 203, 528.
Zirin, H.: 1974, in R. G. Athay (ed.), ‘Chromospheric Fine Structure’, IAU Symp. 56, 161.
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Shibata, K., Suematsu, Y. Why are spicules absent over plages and long under coronal holes?. Sol Phys 78, 333–345 (1982). https://doi.org/10.1007/BF00151612
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DOI: https://doi.org/10.1007/BF00151612