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Abstract
New observational data related to the X1.1/2N solar flare of 17 July 2004 were investigated and compared with some old data for other powerful flares and non-flare regions. Observations were carried out with the Echelle spectrograph of the Kyiv University Astronomical Observatory. The Stokes I ± V profiles of several metallic lines with different effective Lande factors geff have been analyzed including the FeI 5434.5 line with very low magnetic sensitivity (geff = –0.014). The obvious evidences of the emissive Zeeman effect were found as in lines with great and middle Lande factors as in FeI 5434.5 line. On the basis of all analyzed data one can conclude that upper magnetic field limit in flares can reach 70 - 90 kG, i.e. about more order higher than the well-known magnetic fields in great sunspots. The possible physical nature of such superstrong fields is discussed.
Highlights
On the basis of all analyzed data one can conclude that upper magnetic field limit in flares can reach 70 - 90 kG, i.e. about more order higher than the well-known magnetic fields in great sunspots
The upper magnetic field strength limit in the solar atmosphere is unknown at present
The point of view predominates that the strongest fields exist at great sunspots
Summary
The upper magnetic field strength limit in the solar atmosphere is unknown at present. Bruce [7] supposed that long wings of Hα line in flares (till 8 Å) could arise due to the Zeeman effect in 10 - 100 kG fields This is one of possible interpretation: some account to the line-profile broadening should give temperature, turbulent velocity and electric fields. Taking into account that non-flare profiles did not display similar effects, it was assumed the Zeeman effect manifestation in field of B ≈ 26 – 94 kG Such extraordinary conclusion needs an additional and careful verification on a base of new data for other flares. Only unique spectral data are suitable to the problem, related to the suddenly occurred large and bright solar flares Some of such flares were observed on Echelle spectrograph of horizontal solar telescope of Kyiv University astronomical observatory [14]. The new observational data related to the X1.1 solar flare are presented and analyzed
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