A timing formula for main-sequence star binary pulsars

Wex, Norbert

doi:10.1046/j.1365-8711.1998.01570.x

Cited by 50 publications

(86 citation statements)

References 22 publications

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“…In several DNS systems, more than two PK parameters have been measured, which then also allows for a consistency test of the applied gravity theory. So far, general relativity (GR) has passed all these tests with flying colors (Wex 2014), and has therefore been confirmed to be the correct theory to determine the masses from PK parameters in DNS systems.…”

Section: Measuring Ns Massesmentioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

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641

690

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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Section: Measuring Ns Massesmentioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

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641

690

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“…The rotationally induced quadrupole of the companion produces a variation of the orbital inclination angle as (Lai et al 1995;Wex 1998) …”

Section: Origin Of the Variation Of The Projected Semi-major Axismentioning

confidence: 99%

Orbital variability of the PSR J2051-0827 binary system

Doroshenko

Löhmer

Krämer

et al. 2001

A&A

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Abstract.We have carried out high-precision timing measurements of the binary millisecond pulsar PSR J2051−0827 with the Effelsberg 100-m radio telescope of the Max-Planck-Institut für Radioastronomie and with the Lovell 76-m radio telescope at Jodrell Bank. The 6.5-yrs radio timing measurements have revealed a significant secular variation of the projected semi-major axis of the pulsar at a rate ofẋ ≡ d(a1 sin i)/dt = (−0.23 ± 0.03) × 10 −12 , which is probably caused by the Newtonian spin-orbit coupling in this binary system leading to a precession of the orbital plane. The required misalignment of the spin and orbital angular momenta of the companion are evidence for an asymmetric supernova explosion. We have also confirmed that the orbital period is currently decreasing at a rate ofṖ b = (−15.5 ± 0.8) × 10 −12 s s −1 and have measured second and third orbital period derivatives d 2 P b /dt 2 = (+2.1 ± 0.3) × 10 −20 s −1 and d 3 P b /dt 3 = (3.6 ± 0.6) × 10 −28 s −2 , which indicate a quasi-cyclic orbital period variation similar to those found in another eclipsing pulsar system, PSR B1957+20. The observed variation of the orbital parameters constrains the maximal value of the companion radius to Rc max ∼ 0.06 R and implies that the companion is underfilling its Roche lobe by 50%. The derived variation in the quadrupole moment of the companion is probably caused by tidal dissipation similar to the mechanism proposed for PSR B1957+20. We conclude that the companion is at least partially non-degenerate, convective and magnetically active.

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“…Significant classical contributions toω, either from tidal deformation 12 or rotation-induced quadrupole moment 13,14 in the companion -effects which might be present if it were not a neutron star -are therefore unlikely. In fact,ω GR ω would imply an unacceptably low value for the pulsar mass.…”

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An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system

Burgay

D’Amico

Possenti

et al. 2003

Nature

957

845

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The merger 1 of close binary systems containing two neutron stars should produce a burst of gravitational waves, as predicted by the theory of general relativity 2 . A reliable estimate of the double-neutron-star merger rate in the Galaxy is crucial in order to predict whether current gravity wave detectors will be successful in detecting such bursts. Present estimates of this rate are rather low 3−7 , because we know of only a few doubleneutron-star binaries with merger times less than the age of the Universe. Here we report the discovery of a 22-ms pulsar, PSR J0737−3039, which is a member of a highly relativistic double-neutron-star binary with an orbital period of 2.4 hours. This system will merge in about 85 Myr, a time much shorter than for any other known neutron-star binary. Together with the relatively low radio luminosity of PSR J0737−3039, this timescale implies an order-of-magnitude increase in the predicted merger rate for double-neutron-star systems in our Galaxy (and in the rest of the Universe). PSR J0737−3039 was discovered during a pulsar search carried out using a multibeam receiver 8 on the Parkes 64-m radio telescope in New South Whales, Australia. The original detection showed a large change in apparent pulsar period during the 4-min observation time, suggesting that the pulsar is a member of a tight binary system. Follow-up observations undertaken at Parkes consisting of continuous ∼ 5-hour observations showed that the orbit has a very short period (2.4 hrs) and a significant eccentricity (0.088). The derived orbital parameters implied that the system is relatively massive, probably consisting of two neutron stars, and predicted a huge rate of periastron advanceω due to effects of general relativity. Indeed, after only a few days of pulse-timing observations we were able to detect a significant value ofω.Interferometric observations made using the Australia Telescope Compact Array (ATCA) in the 20-cm band gave an improved position and flux density for the pulsar. Knowledge of the pulsar position with subarcsecond precision allowed determination of the rotational period derivative,Ṗ , and other parameters from the available data span. Table 1 reports results derived from a coherent phase fit to data taken over about five months. The measured value ofω = 16.88 • yr −1 is about four times that of PSR B1913+16 (ref. 9), previously the highestknown. If the observedω is entirely due to general relativity, it indicates a total system mass M = 2.58 ± 0.02 M , where M is the mass of the Sun. Figure 1 shows the constraints on the masses of the pulsar and its companion resulting from the observations so far and the mean pulse profile as an inset. The shaded region indicates values that are ruled out by the mass function M f and the observeḋ ω constrains the system to lie between the two diagonal lines. Together, these constraints imply that the pulsar mass m p is less than 1.35 M and that the companion mass m c is greater than 1.24 M . The derived upper limit on m p is consistent with the

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A timing formula for main-sequence star binary pulsars

Cited by 50 publications

References 22 publications

Formation of Double Neutron Star Systems

Formation of Double Neutron Star Systems

Orbital variability of the PSR J2051-0827 binary system

An increased estimate of the merger rate of double neutron stars from observations of a highly relativistic system

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