Advertisement

Abstract

The influence of observer motion and the concomitant Doppler effect on the measured value of a pulsar period is analyzed. A method is given for computing the corrections needed for adjustment of the pulse observations to a barycentric coordinate system.

Keywords

Pulsar Period Ecliptic Plane Moon System Spherical Triangle Observer Motion 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

Preview

Unable to display preview. Download preview PDF.

Unable to display preview. Download preview PDF.

Literature Cited

  1. 1.
    Reference Book of Celestial Mechanics and Astrodynamics [in Russian], Nauka, Moscow (1971).Google Scholar
  2. 2.
    G. M. Clemence and V. Szebenely, Astron. J., 72:1324 (1967).ADSCrossRefGoogle Scholar
  3. 3.
    S. N. Blazhko, Course in Spherical Astronomy [in Russian], Gostekhizdat, Moscow, (1954).Google Scholar
  4. 4.
    L. Ya. Martynov, Course in Practical Astrophysics [in Russian], Fizmatgiz, Moscow (1960).Google Scholar
  5. 5.
    Astronomical Yearbook of the USSR [in Russian], Nauka, Moscow (1975).Google Scholar

Copyright information

© Springer Science+Business Media New York 1979

Authors and Affiliations

  • T. V. Shabanova

There are no affiliations available

Personalised recommendations