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The state of the space environment plays a significant role for forecastingof geomagnetic storms produced by disturbances of the solar wind (SW). Coronalmass ejections (CMEs) passing through the heliosphere often have a prolonged(up to several days) trail with declining speed, which affects propagation ofthe subsequent SW streams. We studied the CME and the post-eruption plasmaflows behind the CME rear in the event on 2010 August 18 observed in quadratureby several space-based instruments. Observations of the eruption in the coronawith EUV telescopes and coronagraphs revealed several discrete outflowsfollowed by a continuous structureless post-eruption stream. The interplanetarycoronal mass ejection (ICME), associated with this CME, was registered byPLAsma and SupraThermal Ion Composition (PLASTIC) instrument aboard the SolarTErrestrial RElations Observatory (STEREO-A) between August 20, 16:14 UT andAugust 21, 13:14 UT, after which the SW disturbance was present over 3 days.Kinematic consideration with the use of the gravitational and Drag-Based modelshas shown that the discrete plasma flows can be associated with the ICME,whereas the post-eruption outflow was arrived in the declining part of the SWtransient. We simulated the Fe-ion charge distributions of the ICME andpost-CME parts of SW using the plasma temperature and density in the ejectionregion derived from the Differential Emission Measure analysis. The resultsdemonstrate that in the studied event the post-ICME trailing region wasassociated with the post-eruption flow from the corona, rather then with theambient SW entrained by the CME.

Formation of Coronal Mass Ejection and Post-eruption Flow of Solar Wind on 2010 August 18 event