Calculation of Intermittency in the Photosphere and Corona From Hinode Data

Details Calculation of Intermittency in the Photosphere and Corona From Hinode Data Calculation of Intermittency in the Photosphere and Corona From Hinode Data

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufmsh34a..05a&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH34A-05

Physics

4440 Fractals And Multifractals, 4475 Scaling: Spatial And Temporal (1872, 3270, 4277), 4490 Turbulence (3379, 4568, 7863), 7509 Corona, 7529 Photosphere

Scientific paper

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.

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