Abstract
The internal kinematics of the Ursa Majoris stellar flow is considered. The details of the flow structure are considered, and new candidate members are searched for using high-precision Gaia DR1 TGAS data. The flow structure is studied using apex diagrams, which have been shown to be effective in studies of open clusters. To select member-stars of the flow, a chain of filters was applied to the spatial coordinates and velocities, photometric data, and elemental abundances of potential members. The nonuniform kinematic structure of the flow, manifest through its separation into different velocity directions for the core and three groups in the corona, is confirmed. Several filters were used to identify three candidate members. These included apex diagrams, MV−(B−V)0 diagrams, and the abundances of Fe, Mg, Al, Si, Ti, and Ni.
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