الفهرس 
Chapter 1: IntroductionOnly 14 pages are availabe for public view
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Abstract
We have studied the relationship between filament disappearances with CMEs and flares during the period 1996-2010. We used the observed disappearing filaments in Hα data from Meudon given in NOAA, solar X-ray flares data from NOAA GEOS satellite, and coronal mass ejections data (CMEs) from SOHO/LASCO.
We obtained 278 CME events (14%) contemporary filament disappearances and CME ejections (from a total of 2018 filament disappearance events and 15,874 CME events during 1996-2010). Only 32% of all filament disappearances were associated with flares. We found that the number of the associated events increased with the increase of the solar activity and significantly decreased with quiet sun. We developed a formula to estimate annual solar X-Ray flares count from annual filament disappearance count.
The longer filament disappearances have activity and ability to contemporary association with CMEs and flares more than shorter filament disappearances. The filament disappearance is source of power of the associated flares and CMEs. CMEs which are associated with filament disappearance are ejected with higher speeds, massive, more energetic, and smaller angular width compared to non-associated CME events. The associated flares have higher solar flux, longer duration, and higher importance compared to non-associated flares with filament disappearance. In addition, the associated filament disappearance with flares or CMEs have two types depending on their duration; short-lived (<9 hours), and long-lived (>9 hours).
We studied the IMF polarity during the minimum solar activity between cycles 20, 21, 22, 23 and 24, and found that it reverses every solar minimum. The correlation between IMFBz and IMFBx is increase with the increase of the solar wind velocity and decrease of the solar wind density. The fast solar winds during the minimum periods we studied were emanated from coronal holes.
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