IJAA  Vol.1 No.3 , September 2011
Observational Evidences for Extremely Strong Magnetic Fields in Solar Flares
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.

Cite this paper
nullV. Lozitsky, "Observational Evidences for Extremely Strong Magnetic Fields in Solar Flares," International Journal of Astronomy and Astrophysics, Vol. 1 No. 3, 2011, pp. 147-154. doi: 10.4236/ijaa.2011.13019.
References
[1]   [1] E. N. Parker, “Solar Activity and Classical Physics,” Chinese Journal on Astronomy and Astrophysics, Vol. 1, No. 2, 2001, pp. 99-124. doi:10.1088/1009-9271/1/2/99

[2]   W. Livingston, J. W. Harvey and O. V. Malanushenko, “Sunspots with the Strongest Magnetic Fields,” Solar Physics, Vol. 239, No. 1, 2006, pp. 41-68. doi:10.1007/s11207-006-0265-4

[3]   N. I. Lozitska and V. G. Lozitsky, “Do Magnetic Transients Exist in Solar Flares?” Soviet Astronomy Letters, Vol. 8, No. 4, 1982, pp. 270-275.

[4]   N. Lozitska and V. Lozitsky, “Small-Scale Magnetic Fluxtube Diagnostics in a Solar Flare,” Solar Physics, Vol.151, No. 2, 1994, pp. 319-331. doi:10.1007/BF00679078

[5]   D. N. Rachkovsky, T. T. Tsap and V. G. Lozitsky, “Small-Scale Magnetic Field Diagnostics Outside Sunspots: Comparison of Different Methods,” Journal of Astrophysics and Astronomy, Vol. 26, No. 4, 2005, pp. 435-445. doi:10.1007/BF02702449

[6]   A. B. Severny, “Some Results of Investigations of Non-Stationare Processes on the Sun,” Astronomicheskii Zhurnal, Vol. 34, No. 5, 1957, pp. 684-693.

[7]   C. E. R. Bruce, “Magnetic Fields in Solar Flares,” Observatory, Vol. 86, No. 951, 1966, pp. 82-83.

[8]   V. G. Lozitsky, “Superstrong Magnetic Fields in the Solar Atmosphere,” Kinematics and Physics of Celestial Bodies, Vol. 9, No. 3, 1993, pp. 18-25.

[9]   V. G. Lozitsky, “Observations of Magnetic Fields with Strengths of Several Tesla in Solar Flares,” Kinematics and Physics of Celestial Bodies, Vol. 14, No. 5, 1998, pp. 307-316.

[10]   V. G. Lozitsky and J. Staude, “Observational Evidences for Multi-Component Magnetic Field Structure in Solar Flares,” Journal of Astrophysics and Astronomy, Vol. 29, No. 3-4, 2008, pp. 387-404. doi:10.1007/s12036-008-0051-9

[11]   V. G. Lozitsky, “Observational Evidences to the 105 G Magnetic Fields in Active Regions on the Sun,” Journal of Physical Studies, Vol. 13, No. 2, 2009, pp. 2903-1- 2903-8.

[12]   E. N. Zemanek and A. P. Stefanov, “Splitting of Some Spectral Lines of FeI in Magnetic Field,” Vestnik Kiev University, Seria Astronomii, No. 18, 1976, pp. 20-36.

[13]   E. L. Landi Degl’Innocenti, “On the Effective Landé Factor of Magnetic Lines,” Solar Physics, Vol. 77, No. 1-2, 1982, pp. 285-289.

[14]   E. V. Kurochka, L. N. Kurochka, V. G. Lozitsky, et al., “Horizontal Solar Telescope of the Kiev University Astronomical Observatory,” Vestnik Kiev University, Seria Astronomii, No. 22, 1980, pp. 48-56.

[15]   V. G. Lozitsky, E. A. Baranovsky, N. I. Lozitska and U. M. Leiko, “Observations of Magnetic Field Evolution in a Solar Flare,” Solar Physics, Vol. 191, No.1, 2000, pp. 171-183. doi:10.1023/A:1005298827306

[16]   R. Howard and J. O. Stenflo, “On the Filamentary Nature of Solar Magnetic Fields,” Solar Physics, Vol. 22, No. 2, 1972, pp. 402-417. doi:10.1007/BF00148705

[17]   H. W. Babcock, “The Solar Magnetograph,” Astrophy- sical Journal, Vol. 118, 1953, pp. 387- 396.

[18]   V. G. Lozitsky, “On the Calibration of Magnetograph Measurements Taking into Account the Spatially Unresolved Inhomogeneties,” Physica Solariterris, Potsdam, No. 14, 1980, pp. 88-94.

[19]   V. G. Lozitsky and T. T. Tsap, “An Empirical Model of the Small-Scale Magnetic Element of the Solar Quiet Region,” Kinematika i Fizika Nebesnykh Tel, Vol. 5, No. 1, 1989, pp. 50-58.

[20]   I. E. Frish, “Optical Spectra of Atoms,” Moscow-Lenin- grad, Fizmatgiz, 1963, p. 640.

[21]   C. E. Moore, “A Multiplet Table of Astrophysical Interest,” Contribution from the Princeton University Observatory, No. 20, Princeton, 1945, p. 96.

[22]   A. A. Soloviev and V. G. Lozitsky, “Force-Free Model of Fine-Structure Magnetic Element,” Kinematika i Fizika Nebesnykh Tel, Vol. 2, No. 5, 1986, pp. 80-84.

 
 
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