Abstract
We present the results from our timing of the millisecond pulsar B1937+21, performed jointly since 1997 on two radio telescopes: the RT-64 in Kalyazin (Russia) at a frequency of 0.6GHz and RT-34 in Kashima (Japan) at a frequency of 2.15 GHz. The rms value of the pulse time of arrival (TOA) residuals for the pulsar at the barycenter of the Solar system is 1.8 μs (the relative variation is ≈10−14 over the observing period). The TOA residuals are shown to be dominated by white phase noise, which allows this pulsar to be used as an independent time scale keeper. The upper limit for the gravitational background energy density Ωg h 2 at frequencies ≈6.5 × 10−9 Hz is estimated to be no higher than 10−6. Based on the long-term timing of the pulsar, we have improved its parameters and accurately determined the dispersion measure and its time variation over the period 1984–2002, which was, on average, −0.00114(3) pc cm−3 yr−1.
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Translated from Pis’ma v Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 31, No. 1, 2005, pp. 33–38.
Original Russian Text Copyright © 2005 by Ilyasov, Imae, Hanado, Oreshko, Potapov, Rodin, Sekido.
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Ilyasov, Y.P., Imae, M., Hanado, Y. et al. Two-frequency timing of the pulsar B1937+21 in Kalyazin and Kashima in 1997–2002. Astron. Lett. 31, 30–36 (2005). https://doi.org/10.1134/1.1854794
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DOI: https://doi.org/10.1134/1.1854794