CSHKP model

CSHKP model is a model of solar flare, which explains flare's observed features on the basis of magnetic reconnection. The basic idea of this model was proposed by the following researchers: Carmichael, Sturrock, Hirayama, Kopp, and Pneuman (Carmichael 1964; Sturrock 1966; Hirayama 1974; Kopp & Pneuman 1976). The model is named CSHKP after these five people. The illustration below shows how the model explains those features observed in Hα, soft and hard X-rays (Magara et al. 1996).

For a quantitative explanation of loop-top source in terms of a standing fast MHD shock wave (perpendicular MHD shock wave), see Section 2.3.2 and Figure 2.6 in Magara, T. 1998, Ph.D. Thesis.


The picture below shows a side view of a Long Duration Event (LDE) flare observed by the SXT telescope on board Yohkoh.


The following movie shows a top view of a two-ribbon flare observed in Hα (pair of white ribbons appeared). This flare was observed on August 29, 1997 at Hida Observatory.


The following movie shows a side view of a flare observed in soft X-ray (an ejecting plasmoid appeared). This flare was observed on September 10, 2017 by Hinode.


References


Carmichael, H. 1964, in AAS-NASA Symposium on Solar Flares, ed. W. N. Hess (NASA SP-50), 451
Hirayama, T. 1974, Sol. Phys., 34, 323
Kopp, R. A., & Pneuman, G. W. 1976, Sol. Phys., 50, 85
Magara, T., Mineshige, S., Yokoyama, T., & Shibata, K. 1996, ApJ, 466, 1054
Sturrock, P. A. 1966, Nature, 211, 695