Titlebook: Eruptive Solar Flares; Proceedings of Collo Zdeněk ?vestka,Bernard V. Jackson,Marcos E. Machad Conference proceedings 1992 Springer-Verlag

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書目名稱Eruptive Solar Flares影響因子(影響力)




書目名稱Eruptive Solar Flares影響因子(影響力)學(xué)科排名




書目名稱Eruptive Solar Flares網(wǎng)絡(luò)公開度




書目名稱Eruptive Solar Flares網(wǎng)絡(luò)公開度學(xué)科排名




書目名稱Eruptive Solar Flares被引頻次




書目名稱Eruptive Solar Flares被引頻次學(xué)科排名




書目名稱Eruptive Solar Flares年度引用




書目名稱Eruptive Solar Flares年度引用學(xué)科排名




書目名稱Eruptive Solar Flares讀者反饋




書目名稱Eruptive Solar Flares讀者反饋學(xué)科排名

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Aggregate

Mechanismus der Kupplungsreaktion,this scenario involves the formation of a filament magnetic field in the corona above a photospheric polarity inversion where cancelling magnetic fields are observed. The formation of a filament magnetic field is accomplished in several recent models by first interpreting the cancelling fields as a

overreach

出血

Hans Euler,Hans Euler,Karl Myrb?ckved the likely location of the separatrices, surfaces that separate cells of different field line connectivities, and of the separator which is the intersection of the separatrices. The connectivity of every magnetic field line, which is defined by the dipoles located at its ends, is computed by a c

出血

TEM

morale

Natürlich vorkommende Insektizideomes to lose its stability and erupt. From observed characteristics (1) of the preflare magnetic field configuration, (2) of the onset and development of the eruption of this configuration before and during the flare, and (3) of the onset and development of the flare energy release (i.e., the heatin

dithiolethione

Definition und Systematik der Bindemittel,prior to the flare becomes opened. One of the requirements of flare models is to explain how the field can be opened while decreasing the overall magnetic energy of the system. After the field is opened, reconnection must occur in order to restore the field to its pre-flare configuration. The strong