Observational Tests of a Double Loop Model for Solar Flares
S. J. Hardy , D. B. Melrose , H. S. Hudson, PASA, 15 (3), 318
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Conclusion

In our exploration of the model of M97 we show that a number of observational tests may be applied to the model to determine the validity of the underlying theory. These include:

1. Any flare event in which the loops structure and footpoint location can be determined may be modeled through the theory of M97. A test based on this geometry may be applied to determine whether or not current transfer leads to energy release, and under what conditions on the currents in the loops. Some geometries are unfavourable for energy release regardless of the current ratio in the loop and flares from such geometries is ruled out by the model.
2. If magnetogram data of sufficient quality has been taken for the active region in which the flare occurs, the currents flowing through the flux loops may be determined. This fully specifies the model of M97, and a comparison between the predicted energy release and the observed energy release may be made.
3. For flares which occur in parasitic geometries, the model of M97 predicts a strong correlation between the energy released in a flare and the ratio of the currents in the interacting loops. This prediction may be tested by examining a number of such flares with a wide range of energies, and looking for correlations between the energy of the flares and the currents in the loops. Application of this approach is hampered by the difficulty in measuring the currents passing through the photosphere directly, and an indirect method of estimating the relative sizes of the currents in the loops may be required.
4. The model of M97 suggests a mechanism for the formation of long flux loops connecting active regions. This mechanism may be tested directly against Yohkoh SXR observations of the formation of these loops.

A number of these observational analyses are under way.

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Next Section: Acknowledgments Title/Abstract Page: Observational Tests of a Previous Section: Application of model

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© Copyright Astronomical Society of Australia 1997