J05101+2733
This star is catalogued as a physical binary, since the two components have similar parallaxes and proper motions. The orbit is probably
physically very large, with a very long period. In fact, the relative position of the stars has not changed since the discovery in 1899. The last
observation dates back from 2015. Since the proper motions of the two stars are very high (0.2"/year in RA and -0.08"/year in DEC), the
motion of each star since 2015 to the present will be approximately 1.8" and 0.7" in RA and DEC, respectively; this will be easily detected if
a multiple observation of the occultation is available. Observers are urged to measure the two contacts if possible.
The B component, in turn, is a spectroscopic binary (the chances are slim that its double nature can be detected in an occultation, but
this is a good oportunity to check).
Given the extremely long separation between the components (315" = 5.2', or just 17% of the Moon's apparent diameter), two separate recordings are
adequate (exposure times can be selected according to the magnitudes of the components). See contact maps for this event.
More information:
www.stelledoppie.it
simbad (A component)
simbad (B component)