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

GAVEL

dyspareunia

defendant

humectant

Definition und Systematik der Bindemittel,vely that these apparent motions are not due to mass motions of the solar plasma. The motions can only be explained by the upward propagation of an energy source in the corona, and in the 1VIHD-reconnection model of flares, the propagating energy source is an x-line accompanied by slow-mode shocks.

投射

Field opening and reconnection,vely that these apparent motions are not due to mass motions of the solar plasma. The motions can only be explained by the upward propagation of an energy source in the corona, and in the 1VIHD-reconnection model of flares, the propagating energy source is an x-line accompanied by slow-mode shocks.

HOWL

Variation of the vector magnetic field in an eruptive flare, established positive field at 0.2 km/s. Data from the JHU/APL vector magnetograph show that this motion led to the development of a sheared field. The flare started near the newly-sheared fields and spread to engulf most of the spot region. A magnetogram taken 45 min after flare onset shows possible relaxation of the sheared fields.

表示向前

Filament eruptions, flaring arches and eruptive flares,ld-up within a day. High resolution H-alpha observations of these events indicate that large amount of ejected material was “siphoned out” from the chromosphere through, the top. of a low-lying compact emission loop within the active region.

foppish

photopsia

脊椎动物

https://doi.org/10.1007/978-3-642-81555-3e chromospheric emission and by the quiet photospheric emission. As a consequence, a temporary decrease of the continuum intensity ( negative flare ) is expected. After less than 20 seconds, the radiative heating of the upper photosphere and temperature minimum region produces a white-light flare.