The Dynamical Parallax of Binaries (L)

Abstract

Let and μ₁ and μ₂ be the masses of the components of a binary, expressed in solar masses. From Newton’s law:

$$ {{\mu }_{1}} + {{\mu }_{2}} = \frac{{{{a}^{3}}}}{{{{P}^{2}}{{p}^{3}}}}, $$

where a is the angular semi-major axis of the relative orbit; p=the parallax, in seconds of arc, P = the period of revolution in years.