Multi-spacecraft Observations of the Coronal and Interplanetary Evolution of a Solar Eruption Associated with Two Active Regions

Abstract

We investigate the coronal and interplanetary evolution of a coronal mass ejection (CME) launched on 2010 September 4 from a source region linking two active regions (ARs) 11101 and 11103, using extreme ultraviolet imaging, magnetogram, white-light and in situ observations from SDO, STEREO, SOHO, VEX and Wind. A potential-field source-surface model is employed to examine the configuration of the coronal magnetic field surrounding the source region. The graduated cylindrical shell model and a triangulation method are applied to determine the kinematics of the CME in the corona and interplanetary space. From the remote sensing and in situ observations we obtain some key results: (1) the CME was deflected in both the eastward and southward directions in the low corona by the magnetic pressure from the two ARs and possibly interacted with another ejection, which caused that the CME arrived at VEX that was longitudinally distant from the source region; (2) although VEX was closer to the Sun, the observed and derived CME arrival times at VEX are not earlier than those at Wind, which suggests the importance of determining both the frontal shape and propagation direction of the CME in interplanetary space; (3) the ICME was compressed in the radial direction while the longitudinal transverse size was extended.

Characteristics of a Gradual Filament Eruption and Subsequent CME Propagation in Relation to a Strong Geomagnetic Storm

“…We use a graduated cylindrical shell (GCS) model proposed byThernisien et al (2006) to fit the CME based on running-difference coronagraph images from STEREO A/COR2and SOHO/LASCO. The GCS model can determine the direction of propagation, tilt angle of CME flux rope and height (e.g.,Thernisien et al 2009;Liu et al 2010b;Hu et al 2017;Zhao et al 2017).Application of the model gives an average propagation direction of about 13 • west of the Sun-Earth line and 6 • north, which is consistent with the location of the flare ribbons (W12 • N17 • ). The speed of the CME leading edge is accelerated from ∼70 km s −1 at 4.4 R ⊙ to ∼370 km s −1 at 16.2 R ⊙ (see below).…”

“…and SOHO/LASCO. The GCS model can determine the direction of propagation, tilt angle of CME flux rope and height (e.g., Thernisien et al 2009;Liu et al 2010b;Hu et al 2017;Zhao et al 2017).…”

Quantifying the Propagation of Fast Coronal Mass Ejections from the Sun to Interplanetary Space by Combining Remote Sensing and Multi-point In Situ Observations

“…The graduated cylindrical shell (GCS) model is a forward modeling technique proposed by Thernisien et al (2006Thernisien et al ( , 2009 and can reproduce CMEs with a croissant-like morphology based on coronagraph observations (e.g., Liu et al 2010Liu et al , 2017Liu et al , 2019Cheng et al 2013;Mishra et al 2015;Hu et al 2017). This model has six free parameters: the longitude and latitude of the propagation direction, the tilt angle, half angle and aspect ratio of the flux rope, and the heliocentric distance of the CME leading front.…”

A Stealth CME Bracketed between Slow and Fast Wind Producing Unexpected Geoeffectiveness

“…The GCS model can determine the direction of propagation, flux rope orientation and height based on the coronagraph images. It has been successfully applied to SOHO/LASCO and STEREO/SECCHI observations (e.g., Thernisien et al 2009;Liu et al 2010bLiu et al , 2017Hu et al 2017;Zhao et al 2017). The GCS model fits the CME observations from the two vantage points very well (see lower panels of Figure 1).…”