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Correlation Length of Energy at the Base of Coronal Holes

Correlation Length of Energy at the Base of Coronal Holes. 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 , AL.

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Correlation Length of Energy at the Base of Coronal Holes

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  1. Correlation Length of Energy at the Base of Coronal Holes Valentina Abramenko 1 Gary Zank2 Alexander Dosch2 Vasyl Yurchyshyn 1 1 - Big Bear solar Observatory of NJIT, CA 2 – CSPAR, Univ. of Alabama in Nuntsville, AL

  2. Photospheric motions are immediately transferred into the chromosphere and corona

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

  4. ux , uy u2

  5. Correlation Function of u2 : 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:

  6. 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.

  7. Calculated Correlation Functions of u2 structures

  8. Parallel and Normal Correlation Functions of ux and uy velocity components

  9. Magnetic Field in Coronal Holes SOT/SP (0.16”) 2007/03/10 HMI (0.5”) 2011/08/12 NST (0.098”) 2012/06/02 16 Mm 120 Mm 36 Mm

  10. Correlation Functions from magnetic field fluctuations

  11. Magnetic and Kinetic Power Specraat the Base of Coronal Holes Valentina Abramenko Big Bear solar Observatory of NJIT, CA

  12. Kinetic and Magnetic Energy Spectra Observed Velocity Spectra

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

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