A Double-Pulsar System: A Rare Laboratory for Relativistic Gravity and Plasma Physics

Lyne, A. G.; Burgay, M.; Krämer, M.; Possenti, A.; Manchester, R. N.; Camilo, F.; McLaughlin, M. A.; Lorimer, D. R.; D’Amico, N.; Joshi, B. C.; Reynolds, John E.; Freire, P. C. C.

doi:10.1126/science.1094645

Cited by 908 publications

(952 citation statements)

References 22 publications

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“…The mass of the BH can be measured with very high accuracy as done for the DNS PSR B1913+16 [41] or the double pulsar [23]. The spin of the BH can also be determined very precisely using the nonlinear-in-time, secular changes in the observable quantities due to relativistic spin-orbit coupling.…”

Section: Pulsar-black Hole Systemsmentioning

confidence: 99%

“…Prime examples are Double-Neutron Star Systems (DNS) such as the famous PSR B1913+16 system [14] or the firstdiscovered double pulsar PSR J0737−3039 [4,23]. As described in more detail in the general description of the pulsar case (Cordes et al, this volume), pulsars enable high-precision tests of GR by probing a number of effects such as the possible violation of equivalence principles, conservation laws or gravitational wave damping.…”

Section: Strong-field Tests Of Gravitymentioning

confidence: 99%

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Strong-field tests of gravity using pulsars and black holes

Krämer

Backer

Cordes

et al. 2004

New Astronomy Reviews

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194

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The sensitivity of the SKA enables a number of tests of theories of gravity. A Galactic Census of pulsars will discover most of the active pulsars in the Galaxy beamed toward us. In this census will almost certainly be pulsarblack hole binaries as well as pulsars orbiting the super-massive black hole in the Galactic centre. These systems are unique in their capability to probe the ultra-strong field limit of relativistic gravity. These measurements can be used to test the Cosmic Censorship Conjecture and the No-Hair theorem.The large number of millisecond pulsars discovered with the SKA will also provide a dense array of precision clocks on the sky. These clocks will act as the multiple arms of a huge gravitational wave detector, which can be used to detect and measure the stochastic cosmological gravitational wave background that is expected from a number of sources.

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Section: Pulsar-black Hole Systemsmentioning

confidence: 99%

Section: Strong-field Tests Of Gravitymentioning

confidence: 99%

Strong-field tests of gravity using pulsars and black holes

Krämer

Backer

Cordes

et al. 2004

New Astronomy Reviews

Self Cite

194

187

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“…This is more complicated in globular clusters: a companion can be dis-rupted by encounter with another star. Direct evidence supporting the MSP spin-up model has been found, for instance, the accreting X-ray MSP SAX J1808.4-3658 (B ∼ 10 8 G, P = 2.49ms) discovered in the low mass X-ray binary system (Wijnands & van den Kils 1998), and the double pulsar PSR 0737-3039A/B (a MSP and a normal PSR in the binary system) (Burgay et al 2003;van den Heuvel 2004;Lyne et al 2004).…”

mentioning

confidence: 99%

Binary pulsars in magnetic field versus spin period diagram

Yuanyue

Wang

Zhang

2013

Astrophys Space Sci

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We analyzed 186 binary pulsars (BPSRs) in the magnetic field versus spin period (B-P) diagram, where their relations to the millisecond pulsars (MSPs) can be clearly shown. Generally, both BPSRs and MSPs are believed to be recycled and spun-up in binary accreting phases, and evolved below the spin-up line setting by the Eddington accretion rate (Ṁ ≃10 18 g/s). It is noticed that most BPSRs are distributed around the spin-up line with mass accretion rateṀ = 10 16 g/s and almost all MSP samples lie above the spin-up line withṀ ∼ 10 15 g/s. Thus, we calculate that a minimum accretion rate (Ṁ ∼ 10 15 g/s) is required for the MSP formation, and physical reasons for this are proposed. In the B-P diagram, the positions of BPSRs and their relations to the binary parameters, such as the companion mass, orbital period and eccentricity, are illustrated and discussed. In addition, for the seven BPSRs located above the limit spin-up line, possible causes are suggested.

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“…This suppression due to decoupling of the anomaly at low frequencies is also the reason why the power radiated in scalar gravitational waves is negligible compared to classical quadrupolar radiation in binary pulsar systems, such as the Hulse-Taylor binary and double pulsar. For the double pulsar the orbital period of 2.454 hours gives an angular frequency ω ≃ 7.11 × 10 −4 sec [67]. This gives a suppression factor in the anomaly source A of ( ω/m e c 2 ) 2 ≃ 2.10 × 10 −49 , which enters the scalar power radiated (6.17) squared.…”

Section: Jhep07(2017)043mentioning

confidence: 99%

Scalar gravitational waves in the effective theory of gravity

Mottola

2017

J. High Energ. Phys.

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As a low energy effective field theory, classical General Relativity receives an infrared relevant modification from the conformal trace anomaly of the energy-momentum tensor of massless, or nearly massless, quantum fields. The local form of the effective action associated with the trace anomaly is expressed in terms of a dynamical scalar field that couples to the conformal factor of the spacetime metric, allowing it to propagate over macroscopic distances. Linearized around flat spacetime, this semi-classical EFT admits scalar gravitational wave solutions in addition to the transversely polarized tensor waves of the classical Einstein theory. The amplitude of the scalar wave modes, as well as their energy and energy flux which are positive and contain a monopole moment, are computed. Astrophysical sources for scalar gravitational waves are considered, with the excited gluonic condensates in the interiors of neutron stars in merger events with other compact objects likely to provide the strongest burst signals.

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A Double-Pulsar System: A Rare Laboratory for Relativistic Gravity and Plasma Physics

Cited by 908 publications

References 22 publications

Strong-field tests of gravity using pulsars and black holes

Strong-field tests of gravity using pulsars and black holes

Binary pulsars in magnetic field versus spin period diagram

Scalar gravitational waves in the effective theory of gravity

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