Binary systems: higher order gravitational radiation damping and wave emission

Junker, W.; Schäfer, Gerhard

doi:10.1093/mnras/254.1.146

Cited by 136 publications

(177 citation statements)

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“…As the tidal interaction between two neutron stars in DNS is extremely weak (Bildsten & Cutler 1992), the major mechanism that changes the orbital semimajor axis and eccentricity of DNS is the emission of gravitational waves. To account for gravitational radiation driven orbital evolution, we use the current observational parameters as initial conditions and integrate Equations (35) and (36) in Junker & Schäfer (1992) backward in time. Because of the uncertainty in the true age of the observed DNS (see Kiziltan & Thorsett 2010 for details), we randomly draw the integration time t i from a uniform distribution of ages between 0 and τ c , where τ c is the characteristic age of the DNS.…”

Section: Methods Of Calculationmentioning

confidence: 99%

Constraints on Natal Kicks in Galactic Double Neutron Star Systems

Wong

Willems

Kalogera

2010

ApJ

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Since the discovery of the first double neutron star (DNS) system in 1975 by Hulse and Taylor, there are currently eight confirmed DNS in our galaxy. For every system, the masses of both neutron stars, the orbital semimajor axis, and eccentricity are measured, and proper motion is known for half of the systems. Using the orbital parameters and kinematic information, if available, as constraints for all systems, we investigate the immediate progenitor mass of the second-born neutron star (NS2) and the magnitude of the supernova kick it received at birth, with the primary goal to understand the core-collapse mechanism leading to neutron star formation. Compared to earlier studies, we use a novel method to address the uncertainty related to the unknown radial velocity of the observed systems. For PSR B1534+12 and PSR B1913+16, the kick magnitudes are 150-270 km s −1 and 190-450 km s −1 (with 95% confidence), respectively, and the progenitor masses of the NS2 are 1.3-3.4 M and 1.4-5.0 M (95%), respectively. These suggest that the NS2 was formed by an iron core-collapse supernova in both systems. For PSR J0737−3039, on the other hand, the kick magnitude is only 5-120 km s −1 (95%), and the progenitor mass of the NS2 is 1.3-1.9 M (95%). Because of the relatively low progenitor mass and kick magnitude, the formation of the NS2 in PSR J0737−3039 is potentially connected to an electron capture supernova of a massive O-Ne-Mg white dwarf. For the remaining five Galactic DNS, the kick magnitude ranges from several tens to several hundreds of km s −1 , and the progenitor mass of the NS2 can be as low as ∼1.5 M or as high as ∼8 M . Therefore, in these systems it is not clear which type of supernova is more likely to form the NS2.

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Section: Methods Of Calculationmentioning

confidence: 99%

Constraints on Natal Kicks in Galactic Double Neutron Star Systems

Wong

Willems

Kalogera

2010

ApJ

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“…In fact, Iyer and Will [10,11] approached this from the opposite direction, beginning with the 1PN accurate flux expressions [26][27][28], and deriving the most general form of a two-body relative equation of motion at 2.5PN and 3.5PN order required by energy and angular momentum balance. Writing the radiation-reaction terms in the equation of motion (1.2) in the general form …”

Section: B 35pn Radiation Reaction and Energy-angular-momentum Balancementioning

confidence: 99%

Post-Newtonian gravitational radiation and equations of motion via direct integration of the relaxed Einstein equations. II. Two-body equations of motion to second post-Newtonian order, and radiation reaction to 3.5 post-Newtonian order

Pati¹,

Will²

2002

Phys. Rev. D

161

147

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We derive the equations of motion for binary systems of compact bodies in the post-Newtonian (PN) approximation to general relativity. Results are given through 2PN order (order (v/c) 4 beyond Newtonian theory), and for gravitational radiation reaction effects at 2.5PN and 3.5PN orders. The method is based on a framework for direct integration of the relaxed Einstein equations (DIRE) developed earlier, in which the equations of motion through 3.5PN order can be expressed in terms of Poisson-like potentials that are generalizations of the instantaneous Newtonian gravitational potential, and in terms of multipole moments of the system and their time derivatives. All potentials are well defined and free of divergences associated with integrating quantities over all space. Using a model of the bodies as spherical, non-rotating fluid balls whose characteristic size s is small compared to the bodies' separation r, we develop a method for carefully extracting only terms that are independent of the parameter s, thereby ignoring tidal interactions, spin effects, and internal self-gravity effects. Through 2.5PN order, the resulting equations agree completely with those obtained by other methods; the new 3.5PN back-reaction results are shown to be consistent with the loss of energy and angular momentum via radiation to infinity.

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“…Using this relation, it is now easy to derive from the eqs. (33) and (35) the leading order contributions [14] …”

Section: Gravitational Waveforms -Analytical Resultsmentioning

confidence: 99%

Motion and gravitational radiation of a binary system consisting of an oscillating and rotating coplanar dusty disk and a point-like object

Hansen

2005

Gen Relativ Gravit

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A binary system composed of an oscillating and rotating coplanar dusty disk and a point mass is considered. The conservative dynamics is treated on the Newtonian level. The effects of gravitational radiation reaction and wave emission are studied to leading quadrupole order. The related waveforms are given. The dynamical evolution of the system is determined semi-analytically exploiting the Hamiltonian equations of motion which comprise the effects both of the Newtonian tidal interaction and the radiation reaction on the motion of the binary system in elliptic orbits. Tidal resonance effects between orbital and oscillatory motions are considered in the presence of radiation damping.

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Binary systems: higher order gravitational radiation damping and wave emission

Cited by 136 publications

References 0 publications

Constraints on Natal Kicks in Galactic Double Neutron Star Systems

Constraints on Natal Kicks in Galactic Double Neutron Star Systems

Post-Newtonian gravitational radiation and equations of motion via direct integration of the relaxed Einstein equations. II. Two-body equations of motion to second post-Newtonian order, and radiation reaction to 3.5 post-Newtonian order

Motion and gravitational radiation of a binary system consisting of an oscillating and rotating coplanar dusty disk and a point-like object

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