Coronal Structure as a Diagnostic of the Solar Dynamo

Details Coronal Structure as a Diagnostic of the Solar Dynamo Coronal Structure as a Diagnostic of the Solar Dynamo

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997spd....28.0151s&link_type=abstract

American Astronomical Society, SPD meeting #28, #01.51; Bulletin of the American Astronomical Society, Vol. 29, p.888

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Scientific paper

This paper is motivated by the discovery of large-scale structures in the distribution of twist of magnetic fields with solar longitude and latitude. These structures are observed to persist for many solar rotations (Pevtsov and Latushko, BAAS 27, 978, 1995; Pevtsov, Canfield, and Metcalf, 4th SOHO Workshop: Helioseismology, Asilomar, 2-6 April 1995; Pevstov, Canfield, and Glatzmaier, Geophysical and Astrophysical Convection, NCAR, 10-13 October 1995). The large scale of these patterns, in space and time, implies that they are a deep-seated phenomenon, presumably that of the solar dynamo itself. Recent observations of twist and tilt of active regions (Pevstov and Canfield, Yohkoh Fifth Anniversary Symposium, Yoyogi, 6-8 November 1996, and Canfield and Pevtsov, this meeting) and the relationship between photospheric and coronal manifestations of twist (Pevstov, Canfield, and McClymont, ApJ 481, in press) confirm this conclusion. The Yohkoh Soft X-Ray Telescope images from the first five years of operations often clearly show the presence of topologically distinct regions. We have developed and used IDL software that allows us to identify and transfer to Carrington coordinates the boundaries of these systems, which we identify with magnetic flux systems. In this paper we present the results of our studies of these systems over many solar rotations, and relate them to the previously discovered persistent large-scale structures in the distribution of twist of active region magnetic fields with longitude and latitude.

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