Search Publications

What are the physical mechanisms of eruptions and CMEs?

Aulanier, Guillaume; Schmieder, Brigitte

CMEs are due to physical phenomena that drive both, eruptions and flares in active regions. Eruptions/CMEs must be driven from initially force-free current-carrying magnetic field. Twisted flux ropes, sigmoids, current lanes and pattern in photospheric current maps show a clear evidence of currents parallel to the magnetic field. Eruptions occur s…

Solar and interplanetary parameters of CMEs with and without type II radio bursts

Moon, Y. -J.; Shanmugaraju, A.; Umapathy, S. +1 more

We have analyzed 101 CMEs, and their associated ICMEs and interplanetary (IP) shocks observed during the period 1997-2005. The main aim of the present work is to study the interplanetary characteristics of metric and DH type II associated CMEs such as, shock strength, IP shock speed, ICME speed, stand off distance and transit time. Among these 101…

Synoptic magnetic field in cycle 23 and in the beginning of the cycle 24

Benevolenskaya, E. E.; Ponyavin, Yu. D.

The SOHO/MDI data provide the uniform time series of the synoptic magnetic maps which cover the period of the cycle 23 and the beginning of the cycle 24. It is very interesting period because of the long and deep solar minimum between the cycles 23 and 24. Synoptic structure of the solar magnetic field shows variability during solar cycles. It is …

MHD simulation of magnetic field configuration above the active region NOAA 10365

Podgorny, I. M.; Podgorny, A. I.

The current sheet (CS) creation before a flare in the vicinity of a singular line above the active region NOAA 10365 is shown in numerical experiments. Such a way the possibility of energy accumulation for a solar flare is demonstrated. These data and results of observation confirm the electrodynamical solar flare model that explains solar flares …

Solar EUV flux variation and flare brightenings

Xie, Wenbin; Bao, Xingming

On 2010 February 8, the Extreme ultraviolet (EUV) flux variation in 195 Å and flare brightening has been examined in different sizes of active regions by using SOHO/EIT, MDI and Hα observational data. These three active regions represent a large active region with a sunspot group, a moderate active region without a sunspot and a small region with …