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Solar energetic particles (SEPs), accelerated during solar eruptions,propagate in turbulent solar wind before being observed with in situinstruments. In order to interpret their origin through comparison withremote-sensing observations of the solar eruption, we thus must deconvolve thetransport effects due to the turbulent magnetic fields from the SEPobservations. Recent research suggests that the SEP propagation is guided bythe turbulent meandering of the magnetic fieldlines across the mean magneticfield. However, the lengthening of the distance the SEPs travel, due to thefieldline meandering, has so far not been included in SEP event analysis. Thisomission can cause significant errors in estimation of the release times ofSEPs at the Sun. We investigate the distance travelled by the SEPs byconsidering them to propagate along fieldlines that meander around closedmagnetic islands that are inherent in turbulent plasma. We introduce afieldline randow walk model which takes into account the physical scalesassociated to the magnetic islands. Our method remedies the problem of thediffusion equation resulting in unrealistically short pathlengths, and thefractal dependence of the pathlength of random walk on the length of therandom-walk step. We find that the pathlength from the Sun to 1 au can be belowthe nominal Parker spiral length for SEP events taking place at solarlongitudes 45E to 60W, whereas the western and behind-the-limb particles canexperience pathlengths longer than 2 au due to fieldline meandering.

From Sun to interplanetary space: What is the pathlength of Solar Energetic Particles?