Abstract
Recently, the Converging Flux Model has been proposed for X-ray bright points and cancelling magnetic features. The aim of this peice of work is to try and model theoretically specific X-ray bright points in the framework of the Converging Flux Model. The observational data used includes a magnetogram showing the normal component of the magnetic field at the photosphere and a high-resolution soft X-ray image from NIXT showing the brightenings in the lower solar corona. By approximating the flux concentrations in the magnetograms with poles of the appropriate sign and sense, the overlying three-dimensional potential field structure is calculated. Deduction of plausible motions of the flux sources are made which produce brightenings of the observed shape due to reconnection between neighbouring flux regions. Also the three-dimensional separarix and separator structure and the way the magnetic field lines reconnect in three dimensions is deduced.
This is a preview of subscription content, log in via an institution to check access.
Similar content being viewed by others
References
Forbes, T. G. and Priest, E. R.: 1984,Solar Phys. 94, 315.
Golub, L., Krieger, A. S., and Vaiana, G. S.: 1976a,Solar Phys. 49, 79.
Golub, L., Krieger, A. S., and Vaiana, G. S.: 1976b,Solar Phys. 50, 311.
Golub, L., Krieger, A. S., Silk, J., Timothy, A. and Vaiana, G.: 1974,Astrophys. J. 189, L93.
Golub, L., Krieger, A. S., Harvey, J., and Vaiana, G.: 1977,Solar Phys. 53, 111.
Harvey, K. L.: 1985,Australian J. Phys. 38, 875.
Heyvaerts, J., Priest, E. R., and Rust, D. M.: 1977,Astrophys. J. 216, 123.
Martin, S. F.: 1984, in S. Keil (ed.),Small-Scale Dynamical Processes in Stellar Atmospheres, Sacramento Peak Observatory, p. 30.
Martin, S. F., Livi, S. H. B., Wang, J., and Shi, Z.: 1984, in M. Hagyard (ed.),Measurements of Solar Vector Magnetic Fields, NASA CP 2374, p. 403.
Priest, E. R., Parnell, C. E., and Martin, S. F.: 1993,Astrophys. J., submitted.
Schmieder, B., Golub, L., and Antiochos, S. K.: 1993, preprint.
Shibata, K., Nozawa, S., and Matsumoto, R.: 1992,Publ. Astron. Soc. Japan 44, 265.
Shibata, K., Ishido, Y., Acton, L., Strong, K., Hirayama, T., Uchida, Y., McAllister, A., Matsumoto, R., Tsuneta, S., Shimizu, T., Hara, H., Sakurai, T., Ichitmoto, K., Nishino, Y., and Ogawara, K.: 1992,Publ. Astron. Soc. Japan 44, L173.
Spiller, E., McCorkle, R. A., Wilczynski, J. S., Golub, L., Nystrom, G., Takacs, P. Z., and Welch, C.: 1991,Opt. Engn. 30, 1109.
Strong, K., Harvey, K., Hirayama, T., Nitta, N., Schimizu, T., and Tsuneta, S.: 1992,Publ. Astron. Soc. Japan 44, L161.
Tsuneta, S. and Lemen, J. R.: 1992, in J. K. Linsky and S. Serio (eds.),Physics of Solar and Stellar Coronae, p. 113.
Tur, T. J. and Priest E. R.: 1976,Solar Phys. 48, 89.
Vaiana, G. S., Krieger, A. S., Van Speybroeck, L. P., and Zehnpfennig, T.: 1970,Bull. Am. Phys. Soc. 15, 611.
Webb, D. F., Martin, S. F., Moses, D., and Harvey, J. W.: 1993,Solar Phys. 144, 15.
Author information
Authors and Affiliations
Rights and permissions
About this article
Cite this article
Parnell, C.E., Priest, E.R. & Golub, L. The three-dimensional structures of X-ray bright points. Sol Phys 151, 57–74 (1994). https://doi.org/10.1007/BF00654082
Received:
Revised:
Issue Date:
DOI: https://doi.org/10.1007/BF00654082