Mathematics – Logic
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52a..03w&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SH52A-03
Mathematics
Logic
7513 Coronal Mass Ejections, 7519 Flares, 7524 Magnetic Fields, 7529 Photosphere, 7536 Solar Activity Cycle (2162)
Scientific paper
The energy of solar flares is released from magnetic fields in solar active regions. Up to now theoretical study has not completely figured out how this energy to be released from solar magnetic fields. Solar flare prediction, therefor, is still based on the statistical relationship between solar flare and magnetic evolution. In order to set up this relationship, sunspot groups are classified according to their morphology and magnetic configuration. For example, there are two kinds of sunspot group classification: Magnetic classification (Alpha, Beta, Beta-Gamma, Gamma Beta/Delta, Beta-Gamma/Delta, Gamma/Delta) and Modified Zurich sunspot class ( A, B, C, D, E, F, G, H, J). It is well known that sunspot groups with Delta type magnetic configuration are very active, in which solar flares occur frequently. However, these classifications provide us limited information on solar active regions. Solar magnetic fields have been measured for long. Evolution of Solar magnetic field can be studied not only morphologically but also quantitatively. Many solar observers have their own experiences for solar flare prediction, since they observed a lot of pre-flare phenomena. Based upon long-term solar magnetic field observation at Huairou Solar Observing Station of Beijing Astronomical Observatory, we proposed the some empirical criteria for solar flare prediction. However, this is not enough to provide short-term solar activity prediction. Nowadays solar photospheric magnetic field observations provide vector magnetic fields on the photospheric surface. Some important physical parameters, such as vertical currents, current helicity, magnetic separatrix, position of singular points and so on, can be derived from the observed magnetic fields. Pre-Status of important solar events must be related to evolutions of these parameters.
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