Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-18T22:17:50.473Z Has data issue: false hasContentIssue false
  • English
  • Français

Model Predictions for Magnetic Shear Changes During Solar Flares

Published online by Cambridge University Press:  12 April 2016

T.G. Forbes
T.G. Forbes*
Affiliation:
Institute for the Study of Earth, Oceans, and Space, University of New Hampshire, Durham, NH 03824, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Magnetic shear is sometimes defined observationally as the rotation of the photospheric vector magnetic field away from the field direction of a corresponding potential state. It is often assumed that the observational shear is a direct measure of the energy stored in coronal currents. However, this is not true in general as is illustrated here by considering the changes in observational shear in a variety of flare models. Some of these models predict rotations in the photospheric transverse field which are too small to be detected by present day instruments, but other models predict relatively large rotations in highly localized regions. In principle, observations of the transverse field might confirm or eliminate models in the latter group.

Type
Session 7. Magnetic Shear and Electric Currents
Information
International Astronomical Union Colloquium , Volume 141: The Magnetic and Velocity Fields of Solar Active Regions , 1993 , pp. 415 - 424
Copyright
Copyright © Astronomical Society of the Pacific 1993

References

Aly, J.J.: 1991, Astrophys. J., 375, L61.Google Scholar
Finn, J.M., and Chen, J.: 1990a, Astrophys. J., 349, 345.Google Scholar
Forbes, T.G.: 1990, J. Geophys. Res., 95, 11919.Google Scholar
Forbes, T.G.: 1991, Geophys. Astrophys. Fluid Dynamics, 62, 15.CrossRefGoogle Scholar
Forbes, T.G., and Isenberg, P.A.: 1991, Astrophys. J., 373, 294.Google Scholar
Forbes, T.G., and Priest, E.R.: 1987, Reviews of Geophys., 25, 1583.Google Scholar
Hagyard, M.J.: 1988, Solar Phys., 115, 107.Google Scholar
Inhester, B., Bim, J., and Hesse, M.: 1992, Solar Phys., 138, 257.Google Scholar
Kan, J.R., Akasofu, S.-I., and Lee, L.C.: 1983, Solar Phys., 84, 153.Google Scholar
Klimchuk, J.A., Canfield, R.C., and Rhoads, J.E.: 1992, Astrophys. J., 385, 327.Google Scholar
Linker, J.A., and Mikic, Z.: 1992, Bull. of the Amer. Astron. Soc., 24, 733.Google Scholar
Low, B.C.: 1985, in Measurements of Solar Vector Magnetic Fields, CP2374, Hagyard, M.J. (ed.), NASA, p. 49.Google Scholar
McClymont, A.N., and Fisher, G.H.: 1989, in Solar System Plasma Physics, Geo-physical Monograph, 54, American Geophysical Union, Washington, D.C., p. 219.Google Scholar
Melrose, D.B., and McClymont, A.N.: 1987, Solar Phys., 113,241.Google Scholar
Priest, E.R., and Forbes, T.G.: 1990, Solar Phys., 130, 399.Google Scholar
Sen, H.K., and White, M.L.: 1972, Solar Phys., 23, 146.Google Scholar
van Ballegooijen, A.A., and Martens, P.C.H.: 1989, Astrophys. J., 343, 971.Google Scholar
Wang, H.: 1992, Solar Phys., 140, 85.CrossRefGoogle Scholar
Wolfson, R., and Low, B.C.: 1992, Astrophys. J., 391, 353.Google Scholar