2023AJ....165..221A

We present detailed analyses of eight triple stellar systems (lying between 20 and 155 pc) and nine quadruple stellar systems (lying between 20 and 250 pc) with different configurations. Most of these systems are hierarchical. The systems are HIP 4239, HIP 5588, HIP 11072, HIP 12548, HIP 13498, HIP 17895, HIP 19915, HIP 22607, HIP 25240, HIP 28614, HIP 41171, HIP 51255, HIP 51966, HIP 54611, HIP 78977, HIP 89234, and HIP 111805. We followed a method that can be applied to all multiple stellar systems, including the main sequence and subgiant evolutionary stages, to obtain their masses, ages, and atmospheric and fundamental parameters. These parameters were assured by the combined analysis of the astrometric measurements, photometric measurements, dynamical analysis, synthetic photometry, metallicity, and positions of the components on the H-R diagram. The estimated individual masses are of higher accuracy than those given by the dynamical solutions and listed in the MSC. The results show that all components of each of these systems have precisely the same age and metallicity. This ensures that fragmentation is the most probable theory for the formation of these multiple stellar systems. A quadratic fit was calculated for the mass-luminosity relation of the main-sequence subset components. We found that the primary component in all of these systems has evolved off the main-sequence stage, and some of these stars have already entered the subgiant stage.