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Energy supply sources for the heating process in the slow solar wind remainunknown. The Parker Solar Probe (PSP) mission provides a good opportunity tostudy this issue. Recently, PSP observations have found that the slow solarwind experiences stronger heating inside 0.24 au. Here for the first time wemeasure in the slow solar wind the radial gradient of the low-frequency breakson the magnetic trace power spectra and evaluate the associated energy supplyrate. We find that the energy supply rate is consistent with the observedperpendicular heating rate calculated based on the gradient of the magneticmoment. Based on this finding, one could explain why the slow solar wind isstrongly heated inside 0.25 au but expands nearly adiabatically outside 0.25au. This finding supports the concept that the energy added from theenergy-containing range is transferred by an energy cascade process to thedissipation range, and then dissipates to heat the slow solar wind. The relatedissues for further study are discussed.

Energy Supply for Heating the Slow Solar Wind Observed by Parker Solar Probe between 0.17 and 0.7 au