||On the Time Variation of the Magnetic Strength Ratio for Different
Combinations of Spectral Lines
||526, Solar Polarization Workshop 8
||Demidov, M. L.; Kiselev, A. V.
||The magnetic strength ratio (MSR) (the ratio of observable strengths Bλ1/Bλ2 in the two spectral lines)
is a good indicator of the
relationship between strong (order of kG)
and weak (no more than a few hG) components of
solar magnetic fields.
Many studies have been devoted to explore the spatial and temporal variations
of the MSR for different combinations
of spectral lines pairs
in order to diagnose solar magnetic fields.
In this investigation we use long-time (1999–2016), multi-lines Solar
Mean Magnetic Field (SMMF) observations made at the STOP
telescope at the Sayan Solar Observatory (SSO).
The SMMF is an important global parameter of solar magnetism, closely
connected with the activity cycle and the distribution of large-scale,
quiet-Sun magnetic fields across the solar disk.
It could be expected that SMMF MSR should show solar cycle variations
due to different contributions
from different magnetic structures.
Instead, our observations have shown only tiny cycle variations. The reason
for that is not clear yet, and new observations are necessary. Additionally,
we present the results of a cross-comparison of SSO and Wilcox Solar observatory
SMMF data sets (SSO measurements in Fe I 5250.2 Å, were used in this case).
Despite two observatories using the same spectral line,
regression coefficients between them show some time variations.