Valentina Abramenko 1 Gary Zank 2 Alexander Dosch 2 Vasyl Yurchyshyn 1 1 - Big Bear solar Observatory of NJIT, CA 2 – CSPAR, Univ. of Alabama in Nuntsville,

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Presentation transcript:

Valentina Abramenko 1 Gary Zank 2 Alexander Dosch 2 Vasyl Yurchyshyn Big Bear solar Observatory of NJIT, CA 2 – CSPAR, Univ. of Alabama in Nuntsville, AL

Magnetic and velocity fluctuations were analyzed in the photosphere inside two coronal holes

u2u2 u x, u y

Correlation Function of u 2 : Correlation function allows to estimate a characteristic length λ of energy containing structures, which defines directly the heating rate: Matthaeus et al. 1999: Zank et al. 2012:

Correlation Function: Correlation function allows to estimate a characteristic length by different ways: 1.To determine the Batchelor integral scale: 2. From an exponential fit to calculate the correlation length ζ 3. To calculate the e-folding scale L of the correlation function.

Calculated Correlation Functions of u 2 structures

Parallel and Normal Correlation Functions of u x and u y velocity components

16 Mm HMI (0.5”) 2011/08/12 SOT/SP (0.16”) 2007/03/10 NST (0.098”) 2012/06/02 36 Mm120 Mm Magnetic Field in Coronal Holes

Correlation Functions from magnetic field fluctuations

Conclusions The characteristic length scale of energy containing structures at the photosphere level seems to be of order of 1000 km (characteristic granule scale), but not km (characteristic super-granular scale) as it was adopted in various SW models so far. Bulk of photospheric dynamics is concentrated in inter-granular lanes.

Valentina Abramenko Big Bear solar Observatory of NJIT, CA

Kinetic and Magnetic Energy Spectra Observed Velocity Spectra

Kinetic and Magnetic Energy Spectra Observed Magnetic Spectra -1/3-1/3 XXV IUGG/IAGA, Melbourne, Australia k -1/3