Figure 6 - On Flare-CME Characteristics from Sun to Earth Combining Remote-Sensing Image Data with In Situ Measurements Supported by Modeling

Time evolution of flare-/CME-related parameters, in comparison to the deduced CME kinematics. a) Distance-, b) velocity-and acceleration-time profile of the CME. c) Reconnected magnetic flux deduced from dimming pixels (211Å211Å) and d) from flare ribbon pixels covering areas of positive (blue) and negative (red) magnetic polarity. Local reconnection rate deduced along different directions of ribbon motion, normal to the local polarity inversion line, from the e) Northern and f) Southern flare ribbon. g) GOES soft X-ray flux (black) and its time derivative (green). Yellow vertical dashed lines mark distinct times within the flare process, including the nominal flare start, peak ("MAX"), and end time. Gray vertical dashed lines mark different phases during the filament eruption.

Go to figure page

Reference

On Flare-CME Characteristics from Sun to Earth Combining Remote-Sensing Image Data with In Situ Measurements Supported by Modeling - Scientific Figure on ResearchGate. Available from: https://www.researchgate.net/figure/Time-evolution-of-flare-CME-related-parameters-in-comparison-to-the-deduced-CME_fig4_328310818 [accessed 22 Jun 2025]

Caption

Figure 6. Time evolution of flare-/CME-related parameters, in comparison to the deduced CME kinematics. a) Distance-, b) velocity-and acceleration-time profile of the CME. c) Reconnected magnetic flux deduced from dimming pixels (211Å211Å) and d) from flare ribbon pixels covering areas of positive (blue) and negative (red) magnetic polarity. Local reconnection rate deduced along different directions of ribbon motion, normal to the local polarity inversion line, from the e) Northern and f) Southern flare ribbon. g) GOES soft X-ray flux (black) and its time derivative (green). Yellow vertical dashed lines mark distinct times within the flare process, including the nominal flare start, peak ("MAX"), and end time. Gray vertical dashed lines mark different phases during the filament eruption.

Embed code

<a href="https://www.researchgate.net/figure/Time-evolution-of-flare-CME-related-parameters-in-comparison-to-the-deduced-CME_fig4_328310818"><img src="https://www.researchgate.net/profile/Karin-Dissauer/publication/328310818/figure/fig4/AS:683084445913094@1539871431794/Time-evolution-of-flare-CME-related-parameters-in-comparison-to-the-deduced-CME.png" alt="Time evolution of flare-/CME-related parameters, in comparison to the deduced CME kinematics. a) Distance-, b) velocity-and acceleration-time profile of the CME. c) Reconnected magnetic flux deduced from dimming pixels (211Å211Å) and d) from flare ribbon pixels covering areas of positive (blue) and negative (red) magnetic polarity. Local reconnection rate deduced along different directions of ribbon motion, normal to the local polarity inversion line, from the e) Northern and f) Southern flare ribbon. g) GOES soft X-ray flux (black) and its time derivative (green). Yellow vertical dashed lines mark distinct times within the flare process, including the nominal flare start, peak ("MAX"), and end time. Gray vertical dashed lines mark different phases during the filament eruption."/></a>