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dc.contributor.authorKopeikin, Sergei M.eng
dc.date.issued2009eng
dc.description.abstractMillisecond 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.eng
dc.identifier.citationarXiv:0909.1054v1eng
dc.identifier.urihttp://hdl.handle.net/10355/6816eng
dc.languageEnglisheng
dc.publisherarXiveng
dc.relation.ispartofcollectionUniversity of Missouri--Columbia. College of Arts and Sciences. Department of Physics and Astronomy. Physics and Astronomy publicationseng
dc.source.urihttp://arxiv.org/PS_cache/arxiv/pdf/0909/0909.1054v1.pdfeng
dc.subjectsolar astrophysicseng
dc.subjectstellar astrophysicseng
dc.subjectinstrumentationeng
dc.subjectmethods for astrophysicseng
dc.subject.lcshPulsars -- Researcheng
dc.subject.lcshPulsarseng
dc.titleStability of pulsar rotational and orbital periodseng
dc.typeArticleeng


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