Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.izmiran.rssi.ru/~obridko/papers/2007ASPC_368_245I Дата изменения: Tue Nov 17 10:38:56 2015 Дата индексирования: Sun Apr 10 02:02:38 2016 Кодировка: Поисковые слова: rosat

The Physics of Chromospheric Plasmas ASP Conference Series, Vol. 368, 2007 Petr Heinzel, Ivan Dorotovi and Robert J. Rutten, eds. c

Some Structural Prop erties of Solar Magnetic Fields
B. Ioshpa, E. Mogilevskii and V. Obridko IZMIRAN, Troitsk, Moscow Region, Russia
Abstract. We discuss some results of the study of spatial characteristics of solar magnetic fields. The analysis is based on the magnetic field data obtained with a new spectromagnetograph installed on the IZMIRAN Tower Telescope (Fe I 6302.5 ° (Kozhevatov et al., 2002), the data of the MSFC solar vector A) magnetograph (Fe I 5250.2 ° and the data of longitudinal magnetic 96 m daily A) maps of SOHO/MDI magnetograph (Ni I 6768 ° downloaded through InterA) net. Our study was directed in some different ways: the fractal properties of sunspots; fractal properties of space distribution of the magnetic fields along great distances comparable with the size of active regions or active complexes; fractal properties of active and quiet regions as global entities. To do it we used some different methods, particularly, the well known method using the relation between the area and the perimeter of magnetic field lines (see (Feder, 1988; Meunier, 1999; Nesme-Ribes at al., 1996; Balke et al., 1993)) and technique developed by Higuchi (1988), who applied it to the investigation of long time series. Note also that magnetic structure in terms of the fractal models was developed earlier in (Zelenyi & Milovanov, 1991; Milovanov & Zelenyi, 1993; Mogilevskii, 1994; Mogilevskii, 2001; Abramenko et al., 2002; Abramenko, 2005; Salakhudinova & Golovko, 2005). The main results are: 1. Fractal analysis of sunspot magnetic field indicated the existence of three families of self-similar contour lines roughly belonging to the umbra, penumbra and the ambient photosphere correspondingly. The greatest fractal dimension corresponds to the regions of weakest fields (ambient photosphere), the least one corresponds to the intermediate region (penumbra). 2. More detailed analysis shows that the fractal coefficient has a maximum (about 1.50) near the umbra­penumbra interface. 3. The global fractal numbers of space distribution of magnetic field on solar surface is closely connected with the mean absolute values of the longitudinal magnetic field for this surface. The fractal numbers diminish with the rising of mean magnetic field (from values about 2.0 for the relatively quiet region to 11.2 for very active regions). 4. The dependences of fractal numbers of the space distribution of longitudinal and transversal fields versus mean longitudinal field are similar by their character but the fractal values for transversal field are higher than the corresponding factor values for longitudinal field by factor about 1.5. This means that the distribution of transversal field along the space is more chaotic than the distribution of longitudinal field.

Acknowledgments. The authors are grateful to the staff of the MSFC vector magnetograph and SOHO/MDI for the data supplied. The work was supported by the RFFI grant 04-02-17007.

245


246
References

Ioshpa et al.

Abramenko, V.I., Yurchyshyn, V.B., Wang, H., Spirock, T.J., & Goode, P.R. 2002, ApJ, 577, 487 Abramenko, V.I. 2005, Solar Phys., 228, 29 Balke, A.C., Schrijver, C.J., Zwaan, C., & Tarbell, T.D. 1993, Solar Phys., 143, 215 Feder, J. 1988, Fractals, Plenum, New York Higuchi, T. 1988, Phisica D, 31, 277 Kozhevatov, I.E., Rudenchik, E.A., Cheragin, N.P., Obridko, V.N., & Kulikova, E.H. 2002, Instruments and Experimental Techniques, 45, No 1, 98 Mandelbrot, B.B. 1983, The Fractal Geometry of Nature, Freeman, New York Meunier, N. 1999, ApJ, 515, 801 Milovanov, A.V., & Zelenyi, L.M. 1992, Phys. Fluids, 5(7), 1406 Mogilevskii, E.I. 1994, Sov. Astron. Lett., 20, N8, 607 Mogilevskii, E.I. 2001, Fractals on the Sun, Fizmatlit Nesme-Ribes, E., Meunier, N., & Collin, D. 1996, A&A, 308, 213 Salakhudinova, I.L., & Golovko, A.A. 2005, Solar Phys., 225, 59 Zelenyi, L.M., & Milovanov, A.V. 1991, Astr. Lett., 17, 425