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 ∼4–20R⊙${\sim}\,4\,\mbox{--}\,20~\mathrm{R}_{\odot }$. 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.

中文翻译：

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将遥感影像数据与建模支持的原位测量相结合，研究从太阳到地球的耀斑-CME 特征

我们分析了自 2011 年 10 月 1 日 (SOL2011-10-01T09:18) 以来观测良好的耀斑和日冕物质抛射 (CME)，涵盖了从太阳到地球的完整效应链，以更好地了解 CME 的动态演变及其嵌入磁场。我们使用太阳动力学天文台 (SDO) 和地面仪器详细研究了与耀斑和 CME 相关的太阳表面和大气。我们还使用来自日地关系天文台 (STEREO) 的组合极紫外 (EUV) 和白光数据跟踪离体 CME 特征。通过将分级圆柱壳 (GCS) 重建方法和总质量应用于立体 STEREO-SOHO（太阳和日光层天文台）日冕仪数据，我们跟踪行星际空间中 CME 的时空演化，并推导出其几何形状和 3D 质量。我们结合 GCS 和 Lundquist 模型结果，从 Wind 的原位测量中推导出磁云 (MC) 的轴向通量和螺旋度。这与非线性无力 (NLFF) 模型结果，以及源自耀斑带的重新连接磁通量（耀斑重新连接通量）和相关调光所包含的磁通量（调光通量）进行了比较。我们发现，在脉冲耀斑阶段开始之前，磁重联过程已经在进行中，在最终爆发之前为磁通绳增加了磁通量。耀斑结束后调光通量增加了25%以上，说明喷发后磁通量绳中仍有磁通量增加。因此，导出的耀斑重联通量很可能是估计磁通绳内磁通量的下限。我们发现行星际空间中的磁螺旋度和轴向磁通量分别降低了约 50% 和 75%，这可能表明存在侵蚀过程。在 ∼4–20R⊙${\sim}\,4\,\mbox{--}\,20~\mathrm{R}_{\odot }$ 范围内观察到 CME 质量增加了 10%。CME 相关核心调光区域的时间演变支持快速流出可能为 CME 后部提供额外质量的情景。在 ∼4–20R⊙${\sim}\,4\,\mbox{--}\,20~\mathrm{R}_{\odot }$ 范围内观察到 CME 质量增加了 10%。CME 相关核心调光区域的时间演变支持快速流出可能为 CME 后部提供额外质量的情景。在 ∼4–20R⊙${\sim}\,4\,\mbox{--}\,20~\mathrm{R}_{\odot }$ 范围内观察到 CME 质量增加了 10%。CME 相关核心调光区域的时间演变支持快速流出可能为 CME 后部提供额外质量的情景。