Astronomy and Astrophysics – Astronomy
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.0601a&link_type=abstract
American Astronomical Society, SPD meeting #40, #6.01; Bulletin of the American Astronomical Society, Vol. 41, p.811
Astronomy and Astrophysics
Astronomy
Scientific paper
Distribution of the magnetic flux inside low-latitude coronal holes (CHs) was analyzed. A statistical study based on SOHO/MDI full disk magnetograms showed that the density of the net magnetic flux does not correlate with the associated solar wind speeds. A possible interpretation is that the density of the magnetic flux derived from the 4 arcsec resolution data is not a suitable parameter to probe energetics in CHs. A reason might be rooted in the structural organization of the magnetic flux, in its fractal nature. As a measure of multifractality of the magnetic field, the filling factor was calculated as a function of spatial scales. The filling factor is independent from scale for a monofractal structure, and it varies with scale for a multifractal structure of burst-like energy release dynamics. Magnetic field filling factor in CHs was found to be nearly constant at scales above 2 Mm, which indicates a monofractal structural organization and smooth temporal evolution. The magnitude of the filling factor is 0.04 from the Hinode SOT/SP data and 0.07 from the MDI/HR data. The Hinode data shows that at scales smaller than 2 Mm, the filling factor decreases rapidly, which means a mutlifractal structure and highly intermittent, burst-like energy release regime. The observed monofractality of the coronal hole magnetic field at scales above 2 Mm seems to be a most plausible reason why the net magnetic flux density does not correlates with the solar wind speed. The bulk of energy release needed for the solar wind acceleration occurs at smaller scales, the scales of multifractality regime, below 1 Mm.
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