A new test of general relativity - Gravitational radiation and the binary pulsar PSR 1913+16

Taylor, J. H.; Weisberg, J. M.

doi:10.1086/159690

Cited by 731 publications

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“…for the eccentricity and for the masses of the two bodies. Therefore, the author feels it plausible that the pulse data of binary pulsars might be nicely fitted by building a timing model entirely based on this theory, in the same way as they have been fitted in GR [25]. What can only be stated for now, is that the theory predicts an energy loss with the same order of magnitude to that which is found in GR and which fits with the observations.…”

Section: Resultsmentioning

confidence: 77%

Gravitational Effects on Light Rays and Binary Pulsar Energy Loss in a Scalar Theory of Gravity

Arminjon¹

2004

Theoretical and Mathematical Physics

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A scalar bimetric theory of gravity with a preferred reference frame is summarized. Dynamics is governed by an extension of Newton's second law. In the static case, geodesic motion is recovered together with Newton's attraction field. In the static spherical case, Schwarzschild's metric is found. Asymptotic schemes of post-Newtonian (PN) and post-Minkowskian (PM) approximation are built, each based on associating a conceptual family of systems with the given system. At the 1PN approximation, there is no preferred-frame effect for photons, hence the standard predictions of GR for photons are got. At the 0PM approximation, an isolated system loses energy by quadrupole radiation, without any monopole or dipole term. Inserting this loss into the Newtonian 2-body problem gives the Peters-Mathews coefficients of the theory.

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Section: Resultsmentioning

confidence: 77%

Gravitational Effects on Light Rays and Binary Pulsar Energy Loss in a Scalar Theory of Gravity

Arminjon¹

2004

Theoretical and Mathematical Physics

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“…The interaction between stars in binaries is responsible for producing a variety of transient phenomena in astrophysics, including, among others, type Ia supernovae (single degenerate: Whelan & Iben 1973;double degenerate: Webbink 1984 andTutukov 1984), gamma-ray bursts (e.g., Brown, Lee, & Moreno Mén-dez 2007;Moreno Méndez et al 2011;Berger 2014), ultraluminous x-ray sources (e.g. Rappaport, Podsiadlowski, & Pfahl 2005;Liu et al 2013), novae (Crawford & Kraft 1956;Darnley et al 2012), millisecond pulsars (Wijnands & van der Klis 1998), gravitational waves (Taylor & Weisberg 1982;Abbott et al 2016), and common envelopes (CE; Ivanova et al 2013), among others.…”

Section: Introductionmentioning

confidence: 99%

Dynamics of jets during the common-envelope phase

Méndez

López-Cámara

Colle

2017

Monthly Notices of the Royal Astronomical Society

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Common envelope (CE) is an important phase in the evolution of many binary systems. Giant star / compact object interaction in binaries plays an important role in highenergy phenomena as well as in the evolution of their environment. Material accreted onto the compact object may form a disk and power a jet. We study analytically and through numerical simulations the interaction between the jet and the CE. We determine the conditions under which accreting material quenches the jet or allows it to propagate successfully, in which case even the envelope may be ejected. Close to the stellar core of the companion the compact object accretes at a larger rate. A jet launched from this region needs a larger accretion-to-ejection efficiency to successfully propagate through the CE compared to a jet launched far from the stellar core, and is strongly deflected by the orbital motion. The energy deposited by the jet may be larger than the binding energy of the envelope. The jet can, thus, play a fundamental role in the CE evolution. We find that the energy dissipation of the jet into the CE may stop accretion onto the disk. We expect the jet to be intermittent, unless the energy deposited is large enough to lead to the unbinding of the outer layers of the CE. Given that the energy and duration of the jet are similar to those of ultra-long GRBs, we suggest this as a new channel to produce these events.

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“…This represents the culmination of a century-long effort that started with Einstein's original descriptions of gravitational waves [2,3] and continued with the demonstration that close binaries with two neutron stars spiral together at the rate predicted by general relativity [4,5,6]. It also represents the beginning of what is expected to be an exploration of a new window to the universe, through which we can see extreme and previously invisible events.…”

Section: Introductionmentioning

confidence: 99%

Implications of the gravitational wave event GW150914

Miller

2016

Gen Relativ Gravit

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The era of gravitational-wave astronomy began on 14 September 2015, when the LIGO Scientific Collaboration detected the merger of two ∼ 30 M ⊙ black holes at a distance of ∼ 400 Mpc. This event has facilitated qualitatively new tests of gravitational theories, and has also produced exciting information about the astrophysical origin of black hole binaries. In this review we discuss the implications of this event for gravitational physics and astrophysics, as well as the expectations for future detections. In brief: (1) because the spins of the black holes could not be measured accurately and because mergers are not well calculated for modified theories of gravity, the current analysis of GW150914 does not place strong constraints on gravity variants that change only the generation of gravitational waves, but (2) it does strongly constrain alterations of the propagation of gravitational waves and alternatives to black holes. Finally, (3) many astrophysical models for the origin of heavy black hole binaries such as the GW150914 system are in play, but a reasonably robust conclusion that was reached even prior to the detection is that the environment of such systems needs to have a relatively low abundance of elements heavier than helium.

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A new test of general relativity - Gravitational radiation and the binary pulsar PSR 1913+16

Cited by 731 publications

References 0 publications

Gravitational Effects on Light Rays and Binary Pulsar Energy Loss in a Scalar Theory of Gravity

Gravitational Effects on Light Rays and Binary Pulsar Energy Loss in a Scalar Theory of Gravity

Dynamics of jets during the common-envelope phase

Implications of the gravitational wave event GW150914

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