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tokens: case, even if the Coulomb collision scenario outlined above was not valid, the waves generated during the magnetic field reconfiguration could discriminate between fully stripped and normal ions for a short time before being dissipated, resulting in a charge state composition similar to the Outlier one. If such a reconnection event occurred high in the corona where the plasma density is low enough, ionization would not be able to replenish the ions left behind, leaving the decrease in their abundance intact. However, if the wave–plasma interaction was depositing energy to all ions except the fully stripped ones, the Outlier wind should exhibit larger ion temperatures in normal ions than in the fully stripped ones. Also, the presence of an additional energy source to this wind, which is unavailable to the normal slow wind and not directly associated with the reconnection region, would cause the ion temperature in the Outlier wind to be larger than in the normal wind. Figure 10 shows, however, quite the opposite: (1) all heavy ions have the same temperatures in the Outlier wind, and (2) these ion temperature values are lower than in the normal slow wind. However, the signatures of wave–plasma interaction at the reconnection point could easily be lost during the Outlier wind propagation in the heliosphere after the initial release, so that the comparison shown by Figure 10 does not necessarily rule out this scenario. The acceleration of ions during magnetic reconnection in solar flares has also been investigated with simulations and analytic studies by Drake et al. ( 2009 ). They found that the ions with a high mass-to-charge ratio can behave like pickup particles and be strongly heated more easily than protons as they cross the reconnection exhaust boundary; the threshold for ions to be heated also depends on the plasma β . Whether the depletion of the fully stripped ions in the Outlier slow wind is attributed to the lack of this type of acceleration needs further exploration. 5. CONCLUSIONS In this work, we have studied the Outlier slow solar wind, a subset of slow solar winds that shows a peculiar charge state distribution, and compared its characteristics to those of the normal slow solar wind. The Outlier wind, initially identified through a C 6+ /C 5+ ratio that is much lower than expected, was found to be a subset of slow solar winds with the same properties and source regions as the latter, with the exception of a very large decrease in the abundance of fully stripped ions, which causes a decrease of C and He abundance, and much lower ion temperatures. We argue that no matter what the Outlier wind origination mechanism is, the source region must be above 1.6 solar radii and the generating process must be episodic. We discuss three possible scenarios that could explain the peculiar properties of the Outlier wind: wave–plasma interaction, depletion already contained in coronal loops, and Coulomb collisions. In the first scenario, waves