Also found in: Wikipedia.
dynamical parallaxAn iterative method used to determine the distance and the mass of a visual binary star, usually from measurements of the orbital period (P years) and apparent mean orbital size (l ″) and an estimate of the mass of the two stars (M 1 + M 2 solar masses). The approximate semimajor axis (a AU) of the orbit is calculated from Kepler's third law: (M 1 + M 2 )P 2 = a 3
The ratio of a /l gives an estimate of the distance of the binary. If the apparent magnitude is known, the absolute magnitude can be deduced from the distance modulus and a more accurate value of total mass is hence obtained using the mass-luminosity relation. The process is repeated as necessary using the corrected mass estimates, an inaccurate estimate in mass leading to a much smaller error in distance.