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A Behavioural Model of the Solar Magnetic Cycle

Published online by Cambridge University Press:  24 July 2018

Milton Munroe*
Affiliation:
Retired Academic, High Wycombe, UK email: MMunroe300@aol.com
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All recent models of solar magnetic cycle behaviour assume that the Ω-effect stretches an existing poloidal magnetic field into a toroidal field using differential rotation (Featherstone and Miesch 2015). The α-effect recycles the toroidal field back to a poloidal field by convection and rotation and this is repeated throughout the cycle. Computer simulations based on that conceptual model still leave many questions unanswered. It has not resolved where the solar dynamo is located, what it is or what causes the differential rotation which it takes for granted. Does this paradigm need changing? The conceptual model presented here examines the sun in horizontal sections, analyses its internal structure, presents new characterizations for the solar wind and structures found and shows how their interaction creates rotation, differential rotation, the solar dynamo and the magnetic cycle.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2018 

References

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