Studies of magnetic fields in the solar photosphere using the line-ratio method |
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| Authors: | E A Baranovskii T T Tsap |
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| Institution: | 1.Crimean Astrophysical Observatory Research Institute,Nauchnyi,Crimea, Ukraine |
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| Abstract: | The longitudinal magnetic field measured using the Fe I λ 525 and Fe I λ 524.7 nm lines and global magnetic field of the sun
differ depending on the observatory. To study the cause of these discrepancies, we calculate the H
‖(525)/H
‖(524.7) ratios for various combinations of magnetic elements and compare them with the corresponding observed values. We use
the standard quiet model of the solar photosphere suggesting that there are magnetic fields of different polarities in the
range between zero and several kilogauss. The magnetic element distribution is found as a function of magnetic field strength
and the parameters of this distribution are determined for which the calculated H
‖(525)/H
‖(524.7) ratio agrees with the observed one. The sigma-components are found to be shifted differently for various points of
the Fe I λ 525 nm profile calculated for the inhomogeneous magnetic field. The farther the point is from the line center,
the larger the sigma-components shift. Such a peculiarity of the profiles may be responsible for the discrepancies in the
measured values of the global magnetic field obtained at different observatories. The increase in modulus of the global magnetic
field during the maxima of solar activity can be due to a larger fraction of magnetic elements with kilogauss magnetic fields. |
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