I refer to:
Innes Cameron Solanki 2011, Max-Planck Institut für Sonnensystemforschung:
http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1106.3417
The authors discuss a correlation of quasi periodic EUV jets observed on 100803 on Solar Dynamics Observatory 211 angstrom images and type III bursts observed in WIND WAVES dynamic spectra, 20 kHz to 13.6 MHz band. The EUV jets correlate with brightening at a small site on the edge of the sunspot umbra, and the brightening with 3-min sunspot intensity oscillations.
"...Conclusions: Active region EUV/X-ray jets and interplanetary electron streams originate on the edge of the sunspot umbra. They form along a current sheet between the sunspot open field and closed field connecting to underlying satellite flux. Sunspot running penumbral waves cause roughly 3-min jet footpoint brightening. The relationship between the waves and jets is less clear..."
Innes Cameron Solanki 2011, Max-Planck Institut für Sonnensystemforschung:
http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1106.3417
The authors discuss a correlation of quasi periodic EUV jets observed on 100803 on Solar Dynamics Observatory 211 angstrom images and type III bursts observed in WIND WAVES dynamic spectra, 20 kHz to 13.6 MHz band. The EUV jets correlate with brightening at a small site on the edge of the sunspot umbra, and the brightening with 3-min sunspot intensity oscillations.
"...Conclusions: Active region EUV/X-ray jets and interplanetary electron streams originate on the edge of the sunspot umbra. They form along a current sheet between the sunspot open field and closed field connecting to underlying satellite flux. Sunspot running penumbral waves cause roughly 3-min jet footpoint brightening. The relationship between the waves and jets is less clear..."