Valentina Abramenko Big Bear Solar Observatory of NJIT

1. HMI: Mar 07/00:00 UT HMI: Mar 08/15:22 UT HMI: Mar 09/18:00 UT MDI: Mar 08/15:08 UT Feb 13/03:00 UT Feb 14/22:48 UT Feb 12/00:00 UT Multi-fractality of Solar Magnetic Fields: New Progress with HMI Valentina Abramenko Big Bear Solar Observatory of NJIT Abstract. The SDO/HMI instrument allows us to address temporal variations of magnetic field parameters. Higher sensitivity, lower noise level and smaller pixel size, as compared to MDI data, improve our estimations of multi-scale parameters of magnetic structures. Here we compare spectra of multi-fractality obrained for the same area on the Sun using the MDI/hires and HMI data. We find that while at scales below 4-5 Mm, MDI does not detect any signature of milti-fractality, HMI data, instead, display a multi-fractal ogranization of the magnetic field. About a day before a strong flare, we observe a period of inflation of multi-fractality (complexity) in the photosphere. AR NOAA 11158 AR NOAA 11166 Spectra from Magnetograms: α Sq(r) = <|B(x+r) – B(r )|q> Indexes of the spectra α κ Flatness Function, S6/(S2)3 Small-scale range 2 -5 Mm : multi-fractality index on small scales κ Spectrum cutoff due to noise MDI Large-scale range 5 – 20 Mm : Multi-fractality index on large scales HMI M6.6 X2.2 An increase of the flatness function with the decreasing scale implies the multi-fractal magnetic field. The degree of multi-fractality at small scales (<5 Mm) is correlated to the flaring productivity of ARs (Abramenko et al.2010,ApJ722). A steep power-law flatness was very poor pronounced in MDI data, whereas it is well detectable in HMI data. Both time profiles (the left – for AR 11166, and the right for AR 11158) show that the multi-fractality index on large scales reflects the overall enlargement of the active region. At the same time, the magnetic power spectrum index, α, and the multi-fractality index on small scales, κ, show a waving behavior with well pronounced peaks in multi-fractality approximately 1-2 days before the strongest (in the AR) flare occurs. Time, days of February 2011 α Time variations of the magnetic power spectrum index α, and the multi-fractality index on small scales, κ, reflect the reorganizations of the magnetic field at small scales. These parameters are not responsible for, say, reinforcement/separation of large sunspots, but they are rather reflect appearance of strong field gradients, extended threads and filament-like magnetic features, inner delta-structures inside the AR, etc. For slow evolving, low-flaring ARs, these parameters are not varying with time. However, for rapidly growing, complex and flaring ARs, there are intriguing peculiarities in their time profiles. Thus, a 1-2 days before the strong flare onset, we observe periods of enhanced multi-fractality in the magnetic field (see plots for ARs 11158 and 11166). Note that for very stable, quiet and low-flaring ARs, the variations in these parameters are much smaller. Indexes of the spectra κ M1.7 X1.5 Time, days of March, 2011