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.


Pulsar Period Ecliptic Plane Moon System Spherical Triangle Observer Motion 
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Literature Cited

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Copyright information

© Springer Science+Business Media New York 1979

Authors and Affiliations

  • T. V. Shabanova

There are no affiliations available

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