Abstract
We analyze the well-observed flare and coronal mass ejection (CME) from 1 October 2011 (SOL2011-10-01T09:18) covering the complete chain of effects – from Sun to Earth – to better understand the dynamic evolution of the CME and its embedded magnetic field. We study in detail the solar surface and atmosphere associated with the flare and CME using the Solar Dynamics Observatory (SDO) and ground-based instruments. We also track the CME signature off-limb with combined extreme ultraviolet (EUV) and white-light data from the Solar Terrestrial Relations Observatory (STEREO). By applying the graduated cylindrical shell (GCS) reconstruction method and total mass to stereoscopic STEREO-SOHO (Solar and Heliospheric Observatory) coronagraph data, we track the temporal and spatial evolution of the CME in the interplanetary space and derive its geometry and 3D mass. We combine the GCS and Lundquist model results to derive the axial flux and helicity of the magnetic cloud (MC) from in situ measurements from Wind. This is compared to nonlinear force-free (NLFF) model results, as well as to the reconnected magnetic flux derived from the flare ribbons (flare reconnection flux) and the magnetic flux encompassed by the associated dimming (dimming flux). We find that magnetic reconnection processes were already ongoing before the start of the impulsive flare phase, adding magnetic flux to the flux rope before its final eruption. The dimming flux increases by more than 25% after the end of the flare, indicating that magnetic flux is still added to the flux rope after eruption. Hence, the derived flare reconnection flux is most probably a lower limit for estimating the magnetic flux within the flux rope. We find that the magnetic helicity and axial magnetic flux are lower in the interplanetary space by ∼ 50% and 75%, respectively, possibly indicating an erosion process. A CME mass increase of 10% is observed over a range of {sim},4,mbox{--},20~mathrm{R}_{odot }. The temporal evolution of the CME-associated core-dimming regions supports the scenario that fast outflows might supply additional mass to the rear part of the CME.
Highlights
Since the launch of the Solar Terrestrial Relations Observatory (STEREO: Howard et al, 2008), the Sun-Earth distance range is covered as never before
The nonlinear force-free (NLFF) coronal magnetic model shows highly twisted magnetic fields along the main photospheric inversion line (PIL) (Figure 2b) that clearly outline the dark filament observed in AIA 304 Å (Figure 2a)
The analysis includes a wealth of data combining remote-sensing and in situ instruments to investigate the complete chain of action for the coronal mass ejection (CME) eruption and its evolution from Sun to Earth
Summary
Since the launch of the Solar Terrestrial Relations Observatory (STEREO: Howard et al, 2008), the Sun-Earth distance range is covered as never before. Studies linking filament and MC characteristics were successfully performed by Bothmer and Schwenn (1998), who related interplanetary magnetic properties of MCs to filament orientation and handedness at the Sun. The helicity of an erupting flux rope is assumed to be conserved during the CME propagation in interplanetary space, enabling us to link MCs observed in situ to their solar sources Compared to already existing studies, we bring new aspects into the dynamic evolution of a CME and its embedded magnetic field by analyzing the solar source region in detail using nonlinear force-free and finite-volume helicity modeling, and deriving the reconnected flux from the CME-associated flare ribbons and dimming areas. We compare the results derived from remote-sensing imagery and in situ measurements and discuss the relationship between the parameters
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