Possible Manifestation of Compact, Stable Dark Matter Objects in the Solar System

Abstract

The study of the possible influence of compact stable dark matter (DM) objects on the formation of solar activity cycles [1] has been continued in relation to a primordial black hole (PBH) with a mass on the order of asteroids or planetary satellites. The numerical calculations used the most accurate astronomical data on the orbits of the planets and asteroids in the Solar System. All the dynamical calculations of the Solar System have been carried out in the post-Newtonian approximation, which is particularly important for calculating the significantly eccentric orbit of PBH, which passes close to (and even inside) the Sun’s surface. Such calculations make it possible to use the Solar System as a detector for a possible dark matter planet. It is known [2] that astronomical ground data limit the total mass of dark matter objects within the orbit of Saturn to no more than \(1.7~\, \times {{10}^{{ - 10}}}\) solar mass (~0.005 mass of the Moon or ~0.4 mass of the asteroid Ceres). It is shown that a PBH with a mass of \(\sim {\kern 1pt} 1~\,\, \times {{10}^{{ - 10}}}\) solar mass (\({{m}_{{{\text{Sun}}}}}\)) in a highly eccentric orbit with a period of 11 years can manifest itself as a trigger of a solar dynamo with a cyclic activity of 11 years. It is also shown that along a particular PBH orbit, the observed variations in solar activity are in good agreement with the available experimental data. Furthermore, the gravitational interaction of such a PBH with the Sun and other planets of the Solar System (in particular with Mercury, Venus, Earth, Mars, Jupiter, and Saturn) leads to an explanation of the Maunder and Dalton minima, and other long-term changes in the amplitudes of the solar activity cycles.