南方基地知识库

The component masses and kinematic parameters of the triple star LHS 1070 are redetermined by using the three-body model. It is shown that the discrepancy between new observations and the two-body fitting results is due to the three-body effects, which justifies the necessity of using the three-body model. Numerical integration shows that the three-body system remains integrated and its hierarchical configuration remains unchanged since the formation of the components. This implies that the triple star may not be formed by a three-body encounter. Also, the possibility that the most massive component is itself a tightly bounded binary is excluded based on the redetermined dynamical mass. The improved dynamical masses of the three components are greatly helpful to constrain at the lower end of the stellar empirical mass-luminosity relation.