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Aims: Our goal is to propagate multiple eruptions - obtained throughnumerical simulations performed in a previous study - to 1 AU and to analysethe effects of different background solar winds on their dynamics and structureat Earth. We also aim to improve the understanding of why some consecutiveeruptions do not result in the expected geoeffectiveness, and how a secondarycoronal mass ejection (CME) can affect the configuration of the preceding one.Methods: Using the 2.5D magnetohydrodynamics (MHD) package of the codeMPI-AMRVAC, we numerically modeled consecutive CMEs inserted in two differentsolar winds by imposing shearing motions onto the inner boundary. The initialmagnetic configuration depicts a triple arcade structure shifted southward, andembedded into a bimodal solar wind. We compared our simulated signatures withthose of a multiple CME event in Sept 2009 using data from spacecraft aroundMercury and Earth. We computed and analysed the Dst index for all thesimulations performed. Results: The observed event fits well at 1 AU with twoof our simulations, one with a stealth CME and the other without. Thishighlights the difficulty of attempting to use in situ observations todistinguish whether or not the second eruption was stealthy, because of theprocesses the flux ropes undergo during their propagation in the interplanetaryspace. We simulate the CMEs propagated in two different solar winds, one slowand another faster one. Only in the first case, plasma blobs arise in the trailof eruptions. Interestingly, the Dst computation results in a reducedgeoeffectiveness in the case of consecutive CMEs when the flux ropes arrivewith a leading positive Bz. When the Bz component is reversed, thegeoeffectiveness increases, meaning that the magnetic reconnections with thetrailing blobs and eruptions strongly affect the impact of the arrivinginterplanetary CME.

Study of the propagation, in situ signatures, and geoeffectiveness of shear-induced coronal mass ejections in different solar winds