Editing Visual binary (section)

===Dynamical parallax===
This method is used solely for binary systems. The mass of the binary system is assumed to be twice that of the Sun. Kepler's Laws are then applied and the separation between the stars is determined. Once this distance is found, the distance away can be found via the arc subtended in the sky, providing a temporary distance measurement. From this measurement and the apparent magnitudes of both stars, the luminosities can be found, and by using the mass–luminosity relationship, the masses of each star. These masses are used to re-calculate the separation distance, and the process is repeated a number of times, with accuracies as high as 5% being achieved. A more sophisticated calculation factors in a star's loss of mass over time.<ref name="double">{{cite book|last=Mullaney|first=James|title=Double and multiple stars and how to observe them|publisher=Springer|date=2005|isbn=1-85233-751-6|url=https://archive.org/details/doublemultiplest0000mull|url-access=registration|page=[https://archive.org/details/doublemultiplest0000mull/page/27 27]|quote=Mass–Luminosity relation distance binary.}}</ref>