HR: 17:20h
AN: SH34A-05    [Abstracts]
TI: Calculation of Intermittency in the Photosphere and Corona From Hinode Data
AU: * Abramenko, V
EM: avi@bbso.njit.edu
AF: Big Bear Solar Observaroty of NJIT, 40386 North Shore Lane, Big Bear City, CA 92314, United States
AU: Yurchyshyn, V
EM: vayur@bbso.njit.edu
AF: Big Bear Solar Observaroty of NJIT, 40386 North Shore Lane, Big Bear City, CA 92314, United States
AB: High spatial and temporal resolution observations of the photospheric magnetic field and solar corona, offered recently by Hinode instrument, provide us a unique opportunity to simultaneously estimate degree of intermittency in the photosphere and the corona and to track their variations in time. To do this, we adopted a flatness-function technique, where the slope of the function defines degree of intermittency. The function itself is calculated as the ratio of the sixth-order structure function to the cube of the second-order structure function. Three independent data sets, that were utilized to calculate the intermittency in the corona (XRT/Hinode, GOES, and Nobeyama 9.4 Hz polarization flux), showed a synchronous increase of intermittency during a 5-day time interval that ends with the occurrence of the X3.4 flare in the NOAA 10930. Photospheric intermittency, calculated from SOT-FG/Hinode magnetograms, peaked approximately 1.5 days before the flare onset. The result allows to suggest a preceding gain of intermittency in the photosphere with a following transport of intermittency into the corona.
DE: 4440 Fractals and multifractals
DE: 4475 Scaling: spatial and temporal (1872, 3270, 4277)
DE: 4490 Turbulence (3379, 4568, 7863)
DE: 7509 Corona
DE: 7529 Photosphere
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting