A second companion of the millisecond pulsar 1620 – 26

Backer, D. C.; Foster, Roger S.; Sallmen, S.

doi:10.1038/365817a0

Cited by 118 publications

(79 citation statements)

References 7 publications

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“…For the highest timing precision the electron column density must be monitored (Phillips & Wolszczan 1992;Backer et al 1993a;Kaspi et al 1994). The uneven electron density distribution leads to refractive and diffractive effects that further complicate the removal of plasma propagation effects (Foster & Cordes 1990;Hu et al 1991).…”

Section: Formulation and Recent Results For Single Pulsarsmentioning

confidence: 99%

“…The observations are conducted every two months at 800 and 1400 MHz. The two frequencies allow removal of time variable dispersion (Backer et al 1993a). This year we introduced new hardware that will allow higher precision measurements, began sampling a significantly larger set of objects (Table 2), and initiated observations with a 26m 'pulsar monitoring telescope'.…”

Section: Pulsar Timing Array Experimentsmentioning

confidence: 99%

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Timing of Millisecond Pulsars

Backer

1996

Symp. - Int. Astron. Union

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Abstract.Arrival times of some millisecond pulsars can be measured with submicrosecond precision. This allows unprecedented measurements of the rotation of these stars, astrometric parameters including proper motion and parallax, motion in binary and complex dynamical systems, perturbations resulting from propagation through small scale turbulence in the interstellar plasma and other effects. In addition to the independent parameters which are required to model each pulsar, there is a set of global parameters that affect the array of pulsars in a correlated manner. These parameters involve the international atomic time scale, the ephemeris of the Earth's orbit and the gravitational wave background and have monopole, dipole and quadrupole and higher order angular signatures, respectively.

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Section: Formulation and Recent Results For Single Pulsarsmentioning

confidence: 99%

Section: Pulsar Timing Array Experimentsmentioning

confidence: 99%

Timing of Millisecond Pulsars

Backer

1996

Symp. - Int. Astron. Union

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“…Most obviously, there is the planetary system around the MSP B1257+12 (Wolszczan & Frail 1992;Konacki & Wolszczan 2003) comprising three moon to Earth-mass planets in ≈ 25 d, 66 d, and 98 day orbits that induce an rms scatter of ≈ 1 ms on the residual TOAs. There is also evidence for a planet in a wide orbit around the globular cluster pulsar B1620−26 and its binary white dwarf companion, inferred from both secular changes in the spin down of the pulsar and evolution of the WD-pulsar orbit (Backer et al 1993;Thorsett et al 1999). This planet was likely captured in a three-body interaction common in the dense cluster environment (Sigurdsson 1993) representing a formation channel that will not be discussed further here.…”

Section: Introductionmentioning

confidence: 99%

An Asteroid Belt Interpretation for the Timing Variations of the Millisecond Pulsar B1937+21

Shannon

Cordes

Metcalfe

et al. 2013

ApJ

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Pulsar timing observations have revealed companions to neutron stars that include other neutron stars, white dwarfs, main-sequence stars, and planets. We demonstrate that the correlated and apparently stochastic residual times of arrival from the millisecond pulsar B1937+21 are consistent with the signature of an asteroid belt having a total mass 0.05 M ⊕ . Unlike the solar system's asteroid belt, the best fit pulsar asteroid belt extends over a wide range of radii, consistent with the absence of any shepherding companions. We suggest that any pulsar that has undergone accretion-driven spin-up and subsequently evaporated its companion may harbor orbiting asteroid mass objects. The resulting timing variations may fundamentally limit the timing precision of some of the other millisecond pulsars. Observational tests of the asteroid belt model include identifying periodicities from individual asteroids, which are difficult; testing for statistical stationarity that become possible when observations are conducted over a longer observing span; and searching for reflected radio emission.

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“…Nearly all of the planets in these systems revolve around only one of the stars. The only exception is the planetary system PSR B1620Ϫ26 (Lyne et al 1988;Backer et al 1993), but this system consists not of normal stars but a pulsar and a white dwarf.…”

Section: Introductionmentioning

confidence: 99%

Microlensing Search for Planets with Two Simultaneously Rising Suns

Han

2008

ApJ

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Among more than 200 extrasolar planet candidates discovered to date, there is no known planet orbiting around normal binary stars. In this Letter, we demonstrate that microlensing is a technique that can detect such planets. Microlensing discoveries of these planets are possible because the planet and host binary stars produce perturbations at a common region around center of mass of the binary stars and thus the signatures of both planet and binary can be detected in the light curves of high-magnification microlensing events. The ranges of the planetary and binary separations of systems for optimal detection vary depending on the planet mass. For a Jupiter-mass planet, we find that high detection efficiency is expected for planets located in the range of ∼1-5 AU from the binary stars which are separated by ∼0.15-0.5 AU.

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A second companion of the millisecond pulsar 1620 – 26

Cited by 118 publications

References 7 publications

Timing of Millisecond Pulsars

Timing of Millisecond Pulsars

An Asteroid Belt Interpretation for the Timing Variations of the Millisecond Pulsar B1937+21

Microlensing Search for Planets with Two Simultaneously Rising Suns

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