inside the area of long-lived trajectories. The filamentary structure around the extended region indicates the chaotic motion of escaping particles.

Fig. \[fig:rtbpl5\] (b) shows the ICM for different solar masses ($M_{\odot}$). Black dots represent $M_{\mathrm{Sun}}=0,$ e.g. RTBP, blue dots $M_{\mathrm{Sun}}=0.6 M_{\odot},$ and red dots $M_{\mathrm{Sun}}=1 M_{\odot}.$ Two well-seen consequences can be observed due to the presence of the Sun. Firstly, the size of the domain of non-escaping trajectories diminishes in case of the larger Sun’s mass. Secondly, the position of this area is shifted outward from Earth. As a consequence of this drift, the location of the $L_5$ point relative to the stable island moves toward its border and beyond. We note that the position of the equilibrium point in the RFBP is situated at a different position as in the RTBP (Gabern & Jorba 2001). Considering this fact, it is worth monitoring the fate of the particle starting from the $L_5$ point ($x_0=-0.914,\;y_0=0.068,
v_{x0}=-0.025,\;v_{y0}=-0.228$) and its neighbourhood.

![ICMs for 1300 days. (a) Black dots represent the initial conditions ($x_{0},y_{0}$) for 90000 trajectories that do not escape the system (RTBP) until $T.$ (b) Non-escaped trajectories for the different mass of the Sun. Black, blue, and red dots correspond to 0 