Nowadays, it is evaluated that the local DM density in the solar system is several orders of magnitude higher than the mean Galactic value [10] so that it could be imagined that the solar system is surrounded by a local subhalo, a suggestion reinforced by recent simulations [11]. Several processes have been postulated to clump DM in the solar system [12, 13, 14, 15, 16, 17, 18, 19]; according to Ref. [20, 21], the existence of the solar system itself might be evidence for a local subhalo. Several studies have been dedicated to placing bounds on the local distribution of DM in our solar system from orbital motions of natural major and minor bodies and artificial probes [22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 20, 34, 35], and electromagnetic wave propagation [36]. It has also been suggested that some proposed and approved space-based missions for fundamental physics may be used to search for local distributions of DM as well [37, 38]. Apart from directly affecting orbital motions and electromagnetic waves propagation, DM may also have other effects on the solar system’s bodies: for example, it may concur to form main-sequence stars like the Sun [39] and accrete on the major planets [40, 21], and affect their internal heats [41, 42]. According to Ref. [40], during its journey along the Galaxy since its birth 4.5 Gyr ago the solar system would have encountered about 203M of DM. In Ref. [39] it is stated that the upper limit to the amount of gravitating DM in the Sun would be 2 − 5% of the total solar mass; by assuming that it somehow accumulated during the Sun’s lifetime2, it is possible to infer a mass increase rate of M*/M = 4.4−11×10−12 yr−1.