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Aims. EXor-type objects are protostars that display powerful UV-opticaloutbursts caused by intermittent and powerful events of magnetosphericaccretion. These objects are not yet well investigated and are quite difficultto characterize. Several parameters, such as plasma stream velocities,characteristic densities, and temperatures, can be retrieved from presentobservations. As of yet, however, there is no information about the magneticfield values and the exact underlying accretion scenario is also underdiscussion.  Methods. We use laboratory plasmas, created by a high power laser impacting asolid target or by a plasma gun injector, and make these plasmas propagateperpendicularly to a strong external magnetic field. The propagating plasmasare found to be well scaled to the presently inferred parameters of EXor-typeaccretion event, thus allowing us to study the behaviour of such episodicaccretion processes in scaled conditions.  Results. We propose a scenario of additional matter accretion in theequatorial plane, which claims to explain the increased accretion rates of theEXor objects, supported by the experimental demonstration of effective plasmapropagation across the magnetic field. In particular, our laboratoryinvestigation allows us to determine that the field strength in the accretionstream of EXor objects, in a position intermediate between the truncationradius and the stellar surface, should be of the order of 100 gauss. This, inturn, suggests a field strength of a few kilogausses on the stellar surface,which is similar to values inferred from observations of classical T Tauristars.

Inferring possible magnetic field strength of accreting inflows in EXor-type objects from scaled laboratory experiments