Other
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...200.3809c&link_type=abstract
American Astronomical Society, 200th AAS Meeting, #38.09; Bulletin of the American Astronomical Society, Vol. 34, p.700
Other
Scientific paper
We study the photosphere/chromosphere energetic connection using a nine hour sequence of SVST images obtained May 30, 1998. The data consist of co-spatial, nearly simultaneous filtergrams of G-band (4305 Å ), Ca II K (3934 Å ), two (6563 Å) Hα channels offset by 0.35 Å and 0.7 Å , and Fe I (6302 Å) magnetograms. The cadence of the G-band and Ca K observations is ~ 30 s; that of the other images is ~ 2 min. The pixel scale is 0.06 Mm and field of view 48 X 48 Mm on the Sun. The filtergram resolution is > 0.2 Mm; that of the magnetograms > 0.3 Mm with single magnetogram sensitivity < 150 G. We have co-registered the images to 1 or 2 pixel accuracy. The number distribution of Ca brightenings and of localized changes in magnetic field strength, measured in standard deviations (σ ) from the image means, present three different characteristic regimes; that of the magnetic ``free energy'' (a derived measure based on the local variance of magnetic field) presents two. Ca brightenings below 3σ show a weak but significant correlation with local magnetic field and free energy. At 3σ the strength of the correlation abruptly increases. Above 5σ no correlation is apparent, but large magnetic field values appear. Using a mask to remove the network areas, the weakest brightenings (<1.5 σ ) show anti-correlation with the magnetic field. For 1.5 σ to 4.5 σ there is no correlation. For selected network examples we follow the time evolution in all observed lines. We find cases in which an increase and then relaxation in the magnetic free energy just precedes a local rise in Ca emission followed by a drop to a lower background level than initially. Work supported in part by NSF-ATM-9987305 and NASA-NAG5-10880.
Berger Thomas E.
Cadavid Carlos A.
Lawrence John K.
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