Orbital Variability in the Eclipsing Pulsar Binary PSR B1957+20

Dec, 1993
9 pages
Published in:
  • Astrophys.J.Lett. 426 (1994) L85
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Abstract: (arXiv)
We have conducted timing observations of the eclipsing millisecond binary pulsar PSR~B1957+20, extending the span of data on this pulsar to more than five years. During this time the orbital period of the system has varied by roughly ΔPb/Pb=1.6×107\Delta P_b/P_b = 1.6 \times 10^{-7}, changing quadratically with time and displaying an orbital period second derivative P¨b=(1.43±0.08)×1018\ddot P_b = (1.43 \pm 0.08) \times 10^{-18}\,s1^{-1}. The previous measurement of a large negative orbital period derivative reflected only the short-term behavior of the system during the early observations: the orbital period derivative is now positive and increasing rapidly. If, as we suspect, the PSR~B1957+20 system is undergoing quasi-cyclic orbital period variations similar to those found in other close binaries such as Algol and RS CVn, then the 0.025M0.025\,M{_\odot} companion to PSR~B1957+20 is most likely non-degenerate, convective, and magnetically active.
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