The structure of the solar magnetic field below the photosphere. I - Adiabatic flux tube models

Details The structure of the solar magnetic field below the photosphere. I - Adiabatic flux tube models The structure of the solar magnetic field below the photosphere. I - Adiabatic flux tube models

Feb 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...106...43v&link_type=abstract

Astronomy and Astrophysics, vol. 106, no. 1, Feb. 1982, p. 43-52. Research supported by the Nederlandse Organisatie voor Zuiver

Astronomy and Astrophysics

Astrophysics

44

Adiabatic Conditions, Magnetic Field Configurations, Magnetic Flux, Photosphere, Solar Magnetic Field, Stellar Models, Convection, Coriolis Effect, Solar Activity, Solar Cycles, Solar Flux, Tubes

Scientific paper

A first approximation for the structure of solar emerged flux tubes is made possible by a model of adiabatic flux tubes rooted in the stable layer below the convective zone. In addition to obtaining an estimate of the horizontal flux system position from the observed photosphere field strength, it is shown that a horizontal drift must occur due to unbalanced tension in the horizontal part of emerged flux tubes. An important new problem, of horizontal flux system initial destabilization, is encountered. It is suggested that the horizontal drift of emerged flux tubes, coupled with the Coriolis effect, may play an essential role in the regenerative process underlying the solar cycle, where flux tubes with following polarity move against the direction of rotation and direct the Coriolis force towards the pole in each hemisphere. It is concluded that the model presented may lead to a better understanding of the solar cycle.

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