Magnetic buoyancy and the solar cycle
Article first published online: 19 DEC 2012
©1979. American Geophysical Union. All Rights Reserved.
Eos, Transactions American Geophysical Union
Volume 60, Issue 50, pages 1028–1029, 11 December 1979
How to Cite
1979), Magnetic buoyancy and the solar cycle, Eos Trans. AGU, 60(50), 1028–1029, doi:10.1029/EO060i050p01028-01.(
- Issue published online: 19 DEC 2012
- Article first published online: 19 DEC 2012
- Cited By
Is solar activity related to magnetic buoyancy? This possibility has been considered recently by solar physicist John H. Thomas of the University of Rochester (Nature, 280, 622–663, 1979) in analyzing the effects of the solar dynamo on variations of the sun's radius and temperature. The solar luminosity is given by L = 4πRS2 σ T4 where RS is the solar radius, and thus a decrease in temperature T could imply radial expansion rather than reduction in luminosity L, as has been suggested. A drop in surface temperature of 1°K could be interpreted as a relative radial increase or expansion of ΔRS/RS ∼ 3 x 104.