Parametrized post-Newtonian gravitational redshift

Krisher, Timothy P.

doi:10.1103/physrevd.48.4639

Cited by 12 publications

(14 citation statements)

References 14 publications

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“…13 Note that Ref. [139] for SLy−e0.50 00 −R4, compared to the prediction of the f -mode frequency of an isolated star, as well as the f -mode frequency including the estimated gravitational redshift due to the star's companion. These curves should only be compared away from the periastron bursts.…”

Section: A Inspiralmentioning

confidence: 97%

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of large eccentricities

Chaurasia¹,

Dietrich²,

Johnson-McDaniel³

et al. 2018

Phys. Rev. D

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As current gravitational wave (GW) detectors increase in sensitivity, and particularly as new instruments are being planned, there is the possibility that ground-based GW detectors will observe GWs from highly eccentric neutron star binaries. We present the first detailed study of highly eccentric BNS systems with full (3+1)D numerical relativity simulations using consistent initial conditions, i.e., setups which are in agreement with the Einstein equations and with the equations of general relativistic hydrodynamics in equilibrium. Overall, our simulations cover two different equations of state (EOSs), two different spin configurations, and three to four different initial eccentricities for each pairing of EOS and spin. We extract from the simulated waveforms the frequency of the f-mode oscillations induced during close encounters before the merger of the two stars. The extracted frequency is in good agreement with f-mode oscillations of individual stars for the irrotational cases, which allows an independent measure of the supranuclear equation of state not accessible for binaries on quasicircular orbits. The energy stored in these f -mode oscillations can be as large as 10 −3 M ∼ 10 51 erg, even with a soft EOS. In order to estimate the stored energy, we also examine the effects of mode mixing due to the stars' offset from the origin on the f -mode contribution to the GW signal. While in general (eccentric) neutron star mergers produce bright electromagnetic counterparts, we find that for the considered cases with fixed initial separation the luminosity decreases when the eccentricity becomes too large, due to a decrease of the ejecta mass. Finally, the use of consistent initial configurations also allows us to produce high-quality waveforms for different eccentricities which can be used as a test bed for waveform model development of highly eccentric binary neutron star systems.

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Section: A Inspiralmentioning

confidence: 97%

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of large eccentricities

Chaurasia¹,

Dietrich²,

Johnson-McDaniel³

et al. 2018

Phys. Rev. D

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“…34 As for terms of order 1=c 4 , a detailed derivation performed in the PPN (parametrized post-Newtonian) framework can be found in Ref. 35-including the contribution due to the rotation of the gravitating body. However, only their order of magnitude is relevant here.…”

Section: The Gravitational Frequency Shiftmentioning

confidence: 99%

On the universality of free fall, the equivalence principle, and the gravitational redshift

Nobili

Lucchesi

Crosta

et al. 2013

American Journal of Physics

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Through the contributions of Galileo, Newton, and Einstein, we recall the universality of free fall (UFF), the weak equivalence principle (WEP), and the strong equivalence principle (SEP), in order to stress that general relativity requires all test masses to be equally accelerated in a gravitational field; that is, it requires UFF and WEP to hold. The possibility of testing this crucial fact with null, highly sensitive experiments makes these the most powerful tests of the theory. Following Schiff, we derive the gravitational redshift from the WEP and special relativity and show that, as long as clocks are affected by a gravitating body like normal matter, measurement of the redshift is a test of UFF/WEP but cannot compete with direct null tests. A new measurement of the gravitational redshift based on free-falling cold atoms and an absolute gravimeter is not competitive either. Finally, we compare UFF/WEP experiments using macroscopic masses as test bodies in one case and cold atoms in the other. We conclude that there is no difference in the nature of the test and that the merit of any such experiment rests on the accuracy it can achieve and on the physical differences between the elements it can test, macroscopic proof masses being superior in both respects

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“…Early pioneering work (Evershed 1931) demonstrated that absorption lines near the solar limb were systematically redshifted, although the measurements did not entirely agree with Einstein's theory as the experiment was too difficult for the instrumentation of the time. Subsequent work (see Vessot et al 1980;LoPresto et al 1991;Krisher, Morabito, & Anderson 1993) yielded results which, within the errors (now 1%), were indistinguishable from Einstein's predictions. While measuring the solar gravitational redshift has been a better means of testing General Relativity than of measuring the mass of the Sun, subsequent gravitational redshift work has been aimed primarily at measuring the masses of white dwarf stars in binaries (e.g.…”

Section: Introductionmentioning

confidence: 62%

Main-Sequence Masses and Radii from Gravitational Redshifts

Hippel

1996

The Astrophysical Journal

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Modern instrumentation makes it possible to measure the mass to radius ratio for main sequence stars in open clusters from gravitational redshifts. For stars where independent information is available for either the mass or the radius, this application of general relativity directly determines the other quantity. Applicable examples are: 1) measuring the radii of solar metallicity main sequence stars for which the mass -luminosity relation is well known, 2) measuring the radii for stars where model atmospheres can be used to determine the surface gravity (the mass to radius squared ratio), 3) refining the massradius relation for main sequence stars, and 4) measuring the change in radius as stars evolve off the main sequence and up the giant branch.

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Parametrized post-Newtonian gravitational redshift

Cited by 12 publications

References 14 publications

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of large eccentricities

Gravitational waves and mass ejecta from binary neutron star mergers: Effect of large eccentricities

On the universality of free fall, the equivalence principle, and the gravitational redshift

Main-Sequence Masses and Radii from Gravitational Redshifts

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