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The propagation of Interplanetary Coronal Mass Ejections (ICMEs) in theheliosphere is influenced by many physical phenomena, related to the internalstructure of the ICME and its interaction with the ambient solar wind andmagnetic field. As the solar magnetic field is modulated by the 11-year dynamocycle, our goal is to perform a theoretical exploratory study to assess thedifference of propagation of an ICME in typical minimum and maximum activitybackgrounds. We define a median representative CME at 0.1~au, using bothobservations and numerical simulations, and describe it using a spheromakmodel. We use the heliospheric propagator European Heliospheric FORecastingInformation Asset (EUHFORIA) to inject the same ICME in two differentbackground wind environments. We then study how the environment and theinternal CME structure impact the propagation of the ICME towards Earth, bycomparison with an unmagnetized CME. At minimum of activity, the structure ofthe heliosphere around the ecliptic causes the ICME to slow down, creating adelay with the polar parts of the ejecta. This delay is more important if theICME is faster. At maximum of activity, a southern coronal hole causes anorthward deflection. For these cases, we always find that the ICME at maximumof activity arrives first, while the ICME at minimum of activity is actuallymore geo-effective. The helicity sign of the ICME is also a crucial parameterbut at minimum of activity only, since it affects the magnetic profile and thearrival time of up to 8 hours.

Impact of the solar activity on the propagation of ICMEs: Simulations of hydro, magnetic and median ICMEs at minimum and maximum of activity