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Reconstruction of Sun-as-Star Magnetic Field Structure and Evolution Using Filament Observations

Published online by Cambridge University Press:  12 April 2016

Dmitri I. Ponyavin
Dmitri I. Ponyavin*
Affiliation:
Institute of Physics, St. Petersburg University, 198904, Russia E-mail: [email protected]

Abstract

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A technique is used to restore the magnetic field of the Sun viewed as star from the filament distribution seen on Hα photographs. For this purpose synoptic charts of the large-scale magnetic field reconstructed by the McIntosh method have been compared with the Sun-asstar solar magnetic field observed at Stanford. We have established a close association between the Sun-as-star magnetic field and the mean magnetic field inferred from synoptic magnetic field maps. A filtering technique was applied to find correlations between the Sun-as-star and large-scale magnetic field distributions during the course of a solar cycle. The correlations found were then used to restore the Sun-as-star magnetic field and its evolution in the late 1950s and 1960s, when such measurements of the field were not being made. A stackplot display of the inferred data reveals large-scale magnetic field organization and evolution. Patterns of the Sun-as-star magnetic field during solar cycle 19 were obtained. The proposed technique can be useful for studying the solar magnetic field structure and evolution during times with no direct observations.

Type
Global Patterns
Information
International Astronomical Union Colloquium , Volume 167: New Perspectives on Solar Prominences , 1998 , pp. 493 - 496
Copyright
Copyright © Astronomical Society of the Pacific 1998

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