Influence of the solar radiation pressure and the Yarkovsky effect on the resonant behavior of asteroids with small perihelion distances

In this paper, the impact of the Yarkovsky effect and solar radiation pressure on the resonant behavior of three asteroids with small perihelion distances (3200 Phaethon, 394130 2006 HY51, and 137924 2000 BD19) is studied. The corresponding physical parameters are determined to estimate the effect of the solar radiation pressure. The Yarkovsky effect and the solar radiation pressure effect are estimated by comparing the results of the orbital evolution of the asteroids with the main force model and the included estimated perturbation. The application of different force models shows that accounting for the Yarkovsky effect and solar radiation pressure has a slight impact on the evolution of the orbital elements of the asteroids while changing the semimajor axis behavior at the ends of the study interval. This impact changes the approaches of the asteroids to planets. It is revealed that the impact of the Yarkovsky effect is stronger than that of the solar radiation pressure. The evolution of the OMEGNO chaoticity parameter shows that the perturbations do not affect the predictability of the motion interval, but in some cases lead to deceleration or acceleration in growth of the parameter. The studied perturbations have no significant effect on the secular (apsidal-nodal) resonance characteristics due to a weak impact on the evolution of the orbital elements underlying their calculations.