Physics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp41c04a&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SP41C-04
Physics
7524 Magnetic Fields, 7529 Photosphere
Scientific paper
We study magnetic power spectra of active and quiet regions by using Big Bear Solar Observatory and SOHO/MDI measurements of longitudinal magnetic fields. The MDI power spectra were corrected with Gaussian Modulation Transfer Function. We obtained reliable magnetic power spectra in the high wave numbers range, up to k=4.6 Mm-1, which corresponds to a spatial scale l=1.4 Mm. We find that the occurrence of the spectral discontinuity at high wavenumbers, k >= 3 Mm-1, largely depends on the spatial resolution of the data and it appears at progressively higher wave numbers as the resolution of the data improves. The spectral discontinuity in the raw spectra is located at wave numbers about 3 times smaller than wavenumbers, corresponding to the resolution of the data, and about 1.5 -- 2.0 times smaller in the case of the noise-and-resolution corrected spectra. The magnetic power spectra for active and quiet regions are different: active region power spectra are described as ~ k-1.7, while in a quiet region the spectrum behaves as ~ k-1.3. We suggest, that the difference can be due to small-scale dynamo action in the quiet sun photosphere. Our estimations show that the dynamo can generate more than 6% of the observed magnetic power.
Abramenko Valentina I.
Goode Philip. R.
Wang Hai-Hong
Yurchyshyn Vasyl
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