Dynamical Parallax

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The Dynamical Parallax is a method of measuring the distance to a visual binary star based on the estimated masses of the two components, the size of the orbit, and the period of their revolution around one another. [1] The angular diameter of the orbit around one of the stars around each other is observed, together with their apparent brightness, and by applying Newton's generalisation of Kepler's Third Law (The squares of the orbital periods of planets are directly proportional to the cubes of the semi-major axis of the orbits) [2] and the Mass-Luminosity relation, the distance to the binary star can be determined. [3]

[edit] References

  1. ^ [1987] Sir Patrick Moore: Astronomy Encyclopædia, Revised (in English), Great Britain: Philip's, 120.
  2. ^ Astronomy Knowledge Base - dynamical parallax (English) (HTML). Astronomy Knowledge Base. Retrieved on 2006-07-18.
  3. ^ The Mass-Luminosity Relation (English) (HTML). Astronomy 162. Retrieved on 2006-07-18.


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