Stability of pulsar rotational and orbital periods
Abstract
Millisecond and binary pulsars are the most stable astronomical standards of frequency. They can be applied to solving a number of problems in astronomy and time-keeping metrology including the search for a stochastic gravitational wave background in the early universe, testing general relativity, and establishing a new time-scale. The full exploration of pulsar properties requires that proper unbiased estimates of spin and orbital parameters of the pulsar be obtained. These estimates depend essentially on the random noise components present in pulsar timing residuals. The instrumental white noise has predictable statistical properties and makes no harm for interpretation of timing observations, while the astrophysical/geophysical low-frequency noise corrupts them, thus, reducing the quality of tests of general relativity and decreasing the stability of the pulsar time scale.
Keywords
Cite
@article{arxiv.0909.1054,
title = {Stability of pulsar rotational and orbital periods},
author = {Sergei Kopeikin},
journal= {arXiv preprint arXiv:0909.1054},
year = {2015}
}
Comments
2 pages, abridged theses of the invited talk at Joint Discussion 6 of XXVII General Assembly of the IAU, Rio de Janeiro, Brazil, August 6-7, 2009 (to appear in Highlights of Astronomy, Vol. 15; edited by Karel van der Hucht)