The Sun and Sun-like stars lose angular momentum to their magnetised stellar winds .
This braking torque is coupled to the stellar magnetic field , such that changes in the strength and/or geometry of the field modifies the efficiency of this process .
Since the space-age , we have been able to directly measure solar wind properties using in-situ spacecraft .
Furthermore , indirect proxies such as sunspot number , geomagnetic indices , and cosmogenic radionuclides , constrain the variation of solar wind properties on centennial , and millennial timescales .
We use near-Earth measurements of the solar wind plasma and magnetic field to calculate the torque on the Sun throughout the space-age .
Then , reconstructions of the solar open magnetic flux are used to estimate the time-varying braking torque during the last nine millennia .
We assume a relationship for the solar mass loss rate based on observations during the space-age which , due to the weak dependence of the torque on mass loss rate , does not strongly affect our predicted torque .
The average torque during the last nine millennia is found to be 2.2 \times 10 ^ { 30 } erg , which is comparable to the average value from the last two decades .
Our dataset includes grand minima ( such as the Maunder Minimum ) , and maxima in solar activity , where the torque varies from \sim 1 - 5 \times 10 ^ { 30 } erg ( averaged on decadal timescales ) , respectively .
We find no evidence for any secular variation of the torque on timescales of less than 9000 years .