Spin-Orbit Couplings in X-Ray Binaries

Tauris, T. M.; Savonije, G. J.

doi:10.1007/978-94-010-0548-7_25

Cited by 199 publications

(471 citation statements)

References 5 publications

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“…In the prerecycling phase, the neutron star has a mass of 1:4 M and the companion a mass m co of 0:8 M , consistent with evolutionary scenarios of low-mass binary pulsars (Tauris & Savonije 1999). The initial semimajor axis of the binary [NS, CO] is 0.03 AU, corresponding to an orbital period P orb;B ¼ 1:3 days, below the bifurcation point (CPG).…”

Section: The Binary Pulsarsupporting

confidence: 59%

Probing the Presence of a Single or Binary Black Hole in the Globular Cluster NGC 6752 with Pulsar Dynamics

Colpi

Mapelli

Possenti

2003

ApJ

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The five millisecond pulsars that inhabit NGC 6752 display locations or accelerations that are quite unusual compared to all other known pulsars in globular clusters. In particular, PSR A, a binary pulsar, lives in the cluster halo, while PSR B and PSR E, located in the core, show remarkably high negative spin derivatives. This suggests that some uncommon dynamical process is at play in the cluster core, which we attribute to the presence of a massive perturber. Here we investigate whether a single intermediate-mass black hole, lying on the extrapolation of the mass M BH versus relation observed in galaxy spheroids, or a less massive binary black hole could play the requested role. To this purpose we simulated binary-binary encounters involving PSR A, its companion star, and the black hole(s). A stellar-mass binary black hole of (50 M ; 10 M ) can impart the right thrust to propel PSR A into the halo during a flyby. The flyby is gentle and does not alter the internal properties of the binary pulsar. An intermediate-mass binary black hole of (200 M ; 10 M ) tends to impart a recoil speed larger than the escape speed: it can release PSR A on the right orbit if its separation is wide. A single intermediate-mass black hole of mass M BH e500 M may have ejected PSR A at the periphery of NGC 6752 in a close dynamical encounter involving the binary pulsar, the black hole, and a star belonging to its cusp. The encounter gives correct speeds but alters significantly the eccentricity of the impinging binary, so that it must occur before the neutron star of PSR A is recycled via accretion torque. The influence of an intermediate-mass binary black hole on the acceleration of the two core pulsars is studied, and the ejection of stars by the binary is briefly explored. In inspecting our close four-body encounters, we have found that a single or binary black hole may attract on a long-term stable orbit a millisecond pulsar. Timing measurements on the captured '' satellite '' pulsar, either a member of a hierarchical triple or a member of the cusp, could unambiguously unveil the presence of a black hole(s) in the core of a globular cluster.

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Section: The Binary Pulsarsupporting

confidence: 59%

Probing the Presence of a Single or Binary Black Hole in the Globular Cluster NGC 6752 with Pulsar Dynamics

Colpi

Mapelli

Possenti

2003

ApJ

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“…The low eccentricity and few-day orbital period of PSR J0740+6620 are consistent with expectations for an He WD companion. A well-defined relationship is observed between P b and M c in such systems (Tauris & Savonije 1999;Istrate et al 2016) and, in the case of PSR J0740+6620, predicts a companion mass M 0.2  . We can also calculate the minimum companion mass by assuming i=90°and M M 1.4 p =  and find M M 0.2 c,min =  .…”

Section: Psr J0740+6620: Constraints On Pulsar and Companion Massmentioning

confidence: 82%

“…The well-known double neutron star (DNS) system PSR B1913+16 provided the first observational evidence for the existence of gravitational waves (GWs; Taylor & Weisberg 1989;Weisberg et al 2010), and the double pulsar system J0737−3039 continues to place ever more stringent constraints on deviations from general relativity (GR) in the strong-field regime (Kramer et al 2006). Neutron star mass measurements can be used to study nuclear physics and the equation of state of ultradense matter (Demorest et al 2010) while also providing insight into the mass distribution of the neutron star population (Özel et al 2012;Kiziltan et al 2013;Antoniadis et al 2016) and, in turn, formation mechanisms and evolution (e.g., Lattimer & Prakash 2004;Tauris & Savonije 1999). Proper-motion measurements can be used to estimate transverse velocity, which also informs theories of neutron star formation and supernova energetics (Ferdman et al 2013).…”

Section: Introductionmentioning

confidence: 99%

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

Lynch

Swiggum

Kondratiev

et al. 2018

ApJ

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We provide timing solutions for 45 radio pulsars discovered by the Robert C. Byrd Green Bank Telescope. These pulsars were found in the Green Bank North Celestial Cap pulsar survey, an all-GBT-sky survey being carried out at a frequency of 350 MHz. We include pulsar timing data from the Green Bank Telescope and Low Frequency Array. Our sample includes five fully recycled millisecond pulsars (MSPs, three of which are in a binary system), a new relativistic double neutron star system, an intermediate-mass binary pulsar, a mode-changing pulsar, a 138 ms pulsar with a very low magnetic field, and several nulling pulsars. We have measured two post-Keplerian parameters and thus the masses of both objects in the double neutron star system. We also report a tentative companion mass measurement via Shapiro delay in a binary MSP. Two of the MSPs can be timed with high precision and have been included in pulsar timing arrays being used to search for low-frequency gravitational waves, while a third MSP is a member of the black widow class of binaries. Proper motion is measurable in five pulsars, and we provide an estimate of their space velocity. We report on an optical counterpart to a new black widow system and provide constraints on the optical counterparts to other binary MSPs. We also present a preliminary analysis of nulling pulsars in our sample. These results demonstrate the scientific return of long timing campaigns on pulsars of all types.

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“…This may be due to the assumptions made on the mass loss rate during the evolution of the secondaries, which was not derived from a detailed physical model. As a matter of fact, the evolutionary calculations by Tauris & Savonije (1999), who included a more sophisticated treatment of mass loss, yield larger maximum radii for the secondaries. It is interesting to note that our assumption of constant envelope mass is not critical because the dependencies on M env cancels each other in the expression for e 2 .…”

Section: Discussionmentioning

confidence: 99%

“…Since the maximum radius is equal to the Roche lobe radius at the end of mass transfer, we can express the semi-major axis and the orbital period as a function of M . More accurate expressions of the massperiod relation are given by King & Ritter (1999) and Tauris & Savonije (1999).…”

Section: The Residual Eccentricitymentioning

confidence: 99%

The residual orbital eccentricity in close binaries

Lanza

Rodonò

2001

A&A

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Abstract. Density fluctuations in convective stars produce small variations of their outer gravitational field that give rise to a very small, though finite, orbital eccentricity in close binaries with convective components. We revisit the theory for such an effect, originally presented by Phinney (1992), and propose a new approach to compute the fluctuations of the outer gravitational field based on Chandrasekhar's virial theorem. It is applied to compute the eccentricities of binaries with a millisecond pulsar component in the framework of a simplified model of their evolution. The comparison with the observations allows us to test the models proposed for the formation of such systems, giving support to the evolutionary scenarios that connect them with low-mass X-ray binaries, and to provide a new test for turbulent convection models of giant stars.

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Spin-Orbit Couplings in X-Ray Binaries

Cited by 199 publications

References 5 publications

Probing the Presence of a Single or Binary Black Hole in the Globular Cluster NGC 6752 with Pulsar Dynamics

Probing the Presence of a Single or Binary Black Hole in the Globular Cluster NGC 6752 with Pulsar Dynamics

The Green Bank North Celestial Cap Pulsar Survey. III. 45 New Pulsar Timing Solutions

The residual orbital eccentricity in close binaries

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