Can We Get the Bottom B?

Details Can We Get the Bottom B? Can We Get the Bottom B?

Mar 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000soph..192...49r&link_type=abstract

Solar Physics, v. 192, Issue 1/2, p. 49-57 (2000).

Physics

3

Scientific paper

Understanding the solar dynamics and the origin of active regions depends crucially on our knowledge of the magnetic fields deep within the convection zone. Can we determine magnetic fields there? Some clues are given by dynamo theories and modeling of those instabilities in the convection zone which result in the emergence of magnetic flux. Magnetic field generated by dynamo is predominantly azimuthal and believed to be unstable to the formation of flux tubes. Simulations indicate that the emergence of the magnetic flux tubes strongly depends on the field strength and its longitudinal distribution at the bottom of the convection zone. In a unifying approach advocated in this paper the solar magnetic field is split into a mean part generated by the mean-field dynamo and a fluctuating part approximated by an ensemble of flux tubes. Observationally, the identification of the longitudinal distribution of emerging photospheric magnetic fields can give us information about the magnetic field strength at the bottom of the convection zone. Distinguishing between the modes of emerging field requires simultaneous magnetic imaging of both sides of the Sun. Correlation of simultaneous Dopplergrams of the photosphere from earthside and from the farside of the Sun opens an opportunity to detect velocity structures at the base of the convection zone, associated with the dynamo and emerging active regions. This global imaging of the photosphere can also be used for detection of a magnetic field in the solar core.

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