Stokes-Meter Observations of the Solar Mean Magnetic Field: Probable Manifestations of Strong Small-Scale Magnetic Fields

Details Stokes-Meter Observations of the Solar Mean Magnetic Field: Probable Manifestations of Strong Small-Scale Magnetic Fields Stokes-Meter Observations of the Solar Mean Magnetic Field: Probable Manifestations of Strong Small-Scale Magnetic Fields

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005arep...49..559d&link_type=abstract

Astronomy Reports, vol. 49, Issue 7, p.559-566

Astronomy and Astrophysics

Astronomy

1

Scientific paper

For many years, information on the solar mean magnetic field (SMMF) of the Sun—an important heliophysical and astrophysical parameter—was restricted to magnetographic measurements in only one spectral line, FeI λ525.02 nm. More informative observations of the Stokes-meter parameters of the SMMF were first initiated on a regular basis at the Sayan Solar Observatory. The availability of I and V data obtained simultaneously in several spectral lines has made it possible to study fundamentally new physical problems. In this paper, based on a comparison of SMMF observations in several spectral lines, we find high correlations in the data and important systematic differences in the magnetic-field strength B, which we interpret as a manifestation of kilogauss magnetic fields in fine-structure magnetic elements. Results of theoretical modeling of the SMMF strength ratios for the FeI λ525.02 nm-FeI λ524.70 nm and FeI λ630.15 nm-FeI λ630.25 nm lines are presented. The asymmetries of the V profiles of four lines near the FeI λ525.02 nm line are examined; these lines are important diagnostics for studies of small-scale dynamical processes. The Sayan Solar Observatory SMMF measurements are in good consistency with the Wilcox Solar Observatory data for 2003: for a comparison of N = 137 pairs of points in the two data sets, the correlation coefficient ρ is 0.92 for the linear regression between the datasets B WSO = 0.03(±0.05) + 0.93(±0.03)B SSO.

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