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A wide class of scalar field models including Quintessence and K-essence havethe attractive property of tracker regimes, where the energy density stored inthe field evolves so as to mimic that of the dominant background component fora period of time. During this evolution, for a brief period of time there is anincrease in the energy density of the field as it spirals in towards it'sattractor solution. We show that when the peak of this energy density occursaround the epoch of equality, we can address a key requirement of early darkenergy (EDE), postulated as a solution to the Hubble tension. In particular wedemonstrate how this can occur in a wide class of Quintessence, axion andK-essence models, before showing that the Quintessence models suffer in thatthey generally lead to sound speeds incompatible with the requirements of EDE,whereas the K-essence and axion models can do a better job of fitting the data.

Scaling solutions as Early Dark Energy resolutions to the Hubble tension