Valentina Abramenko 1 Gary Zank 2 Alexander Dosch 2 Vasyl Yurchyshyn 1 1 - Big Bear solar...

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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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Transcript of Valentina Abramenko 1 Gary Zank 2 Alexander Dosch 2 Vasyl Yurchyshyn 1 1 - Big Bear solar...

Page 1: 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,

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

Page 2: 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,

Photospheric motions are immediately transferred into the chromosphere and corona

Page 3: 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,

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

Page 4: 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,
Page 5: 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,

u2

ux , uy

Page 6: 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,

Correlation Function of u2 :

Correlation function allows to estimate a characteristic length λof energy containing structures, which defines directly the heating rate:

Matthaeus et al. 1999:

Zank et al. 2012:

Page 7: 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,

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.

Page 8: 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,

Calculated Correlation Functions of u2 structures

Page 9: 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,
Page 10: 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,

Parallel and Normal Correlation Functions of ux and uy velocity components

Page 11: 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,

16 Mm

HMI (0.5”) 2011/08/12

SOT/SP (0.16”) 2007/03/10NST (0.098”) 2012/06/02

36 Mm120 Mm

Magnetic Field in Coronal Holes

Page 12: 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,

Correlation Functions from magnetic field fluctuations

Page 13: 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,

Magnetic and Kinetic Power Specra

at the Base of Coronal Holes

Valentina Abramenko Big Bear solar Observatory of NJIT, CA

Page 14: 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,

Kinetic and Magnetic Energy SpectraObserved Velocity Spectra

Page 15: 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,

Kinetic and Magnetic Energy SpectraObserved Magnetic Spectra

-1/3

XXV IUGG/IAGA, Melbourne, Australia

k-1/3


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