Global Electrodynamic Coupling in Stellar Atmospheres
It is now known that the dominant source of star-to-star variation in the level of chromospheric and coronal activity is star-to-star variation in the area covered by magnetic fields (i.e. the magnetic filling factor). Thus, detailed studies of the origin of chromospheric and coronal heating need to look beyond such variations if they are to explore the physical mechanisms that produce different heating rates in different parts of the atmosphere. One way to do this is to study flux-flux relations obtained either from spatially resolved solar observations or stellar data. Here, we offer a simple geometric interpretation of observed flux-flux relations that may shed some light on the nature of electrodynamic coupling in the atmospheres of the Sun and stars.
KeywordsConvection Flare Advection Cote nAph
Unable to display preview. Download preview PDF.
- Gold, T.: 1961, in AAS-NASA Symposium on the Physics of Solar Flares, ed. W.N. Hess (NASA SP-50), p. 389.Google Scholar
- Schrijver, C.J.: 1986, Ph.D. thesis, University of Utrecht.Google Scholar
- Schrijver, C.J., Zwaan, C., Maxson, C.W. & Noyes, R.W.: Astron. Astrophys. 149, 123.Google Scholar
- Schrijver, C.J., Harvey, K.L.: 1990, Ap. J. (in press).Google Scholar
- Spruit, H.C.: 1981, in The Sun as a Star, ed. S.D. Jordan (NASA SP-450), p385.Google Scholar