Current status of gravitational wave observations

Fairhurst, S.; Guidi, G. M.; Hello, P.; Woan, G.

doi:10.1007/s10714-010-1009-1

Cited by 10 publications

(15 citation statements)

References 148 publications

(117 reference statements)

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“…Our calculations are valid, in principle, also for other natural systems like extrasolar planets 4 [74] many of which have orbital frequencies of the order of 10 À4 Hz, orbiting their parent stars at distances as small as ≃ 0.01 au. In such cases, our findings are technically valid for waves with higher frequencies with respect to the solar system ones; indeed, they might be as high as about 5 …”

mentioning

confidence: 57%

“…(1). 5 However, for waves with such relatively high frequencies other facilities like LISA would be available: if they will finally become operative at the expected level of accuracy, they would likely surpass the possibilities offered by the extrasolar planets. 6 In eq.…”

Section: The Acceleration Imparted On An Orbiting Planet By a Passingmentioning

confidence: 99%

“…Indeed, since GTR relies upon the Lorentz invariance, which carries with it the concept of a limiting speed for physical interactions, the existence of gravitational waves is a natural consequence of it. A direct measurement of them is still lacking; see, e.g., Cerdonio [3]; Giazotto [4]; Fairhurst et al [5] for recent reviews of the status of gravitational wave detection. To date, only indirect evidences of their existence have been inferred from the orbital decay rate of the binary pulsar PSR B1913+16 [6] and, more recently, from the detection [7] of B -mode polarization at degree angular scales in the Cosmic Microwave Background (CMB) by the ground-based experiment BICEP2 [8] at the South Pole.…”

Section: Introductionmentioning

confidence: 99%

“…The space-based LISA mission 1 [24][25][26], now evolved into eLISA 2 [27], aimed to detect gravitational waves in the frequency range 10 5 1 Hz, while accurate timing measurements of pulsars may detect signals in the range 10 9 10 7 Hz [28][29][30]. Section 6.2 of Flanagan and Hughes [1] yields an overview of typical LISA sources: they include, e.g., equal mass binaries, in which the member black holes are of roughly equal mass (~10 5 10 8 M ⊙ ), and extreme mass ratio binaries made by white dwarfs, neutron stars and 10100M ⊙ black holes captured by 10 5 10 7 M ⊙ black holes, located at quite large distances. As far as the very low-frequency band is concerned (10 9 10 7 Hz), refer Section 6.3 of Flanagan and Hughes [1].…”

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confidence: 99%

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Orbital effects of a monochromatic plane gravitational wave with ultra-low frequency incident on a gravitationally bound two-body system

Efroimsky¹

2014

ScienceOpen Research

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We analytically compute the long-term orbital variations of a test particle orbiting a central body acted upon by an incident monochromatic plane gravitational wave. We assume that the characteristic size of the perturbed two-body system is much smaller than the wavelength of the wave. Moreover, we also suppose that the wave's frequency n g is much smaller than the particle's orbital one n b . We make neither a priori assumptions about the direction of the wavevector b k nor on the orbital configuration of the particle. While the semi-major axis a is left unaffected, the eccentricity e, the inclination I, the longitude of the ascending node Ω, the longitude of pericenter ϖ and the mean anomaly M undergo non-vanishing long-term changes of the form dW=dt ¼ FðK ij ; e; I; X; xÞ; W ¼ e; I; X; -; M, where K ij ; i; j ¼ 1; 2; 3 are the coefficients of the tidal matrix K. Thus, in addition to the variations of its orientation in space, the shape of the orbit would be altered as well. Strictly speaking, such effects are not secular trends because of the slow modulation introduced by K and by the orbital elements themselves: they exhibit peculiar long-term temporal patterns which would be potentially of help for their detection in multidecadal analyses of extended data records of planetary observations of various kinds. In particular, they could be useful in performing independent tests of the inflation-driven ultra-low gravitational waves whose imprint may have been indirectly detected in the Cosmic Microwave Background by the Earthbased experiment BICEP2. Our calculation holds, in general, for any gravitationally bound two-body system whose orbital frequency n b is much larger than the frequency n g of the external wave, like, e.g., extrasolar planets and the stars orbiting the Galactic black hole. It is also valid for a generic perturbation of tidal type with constant coefficients over timescales of the order of the orbital period of the perturbed particle.

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mentioning

confidence: 57%

Section: The Acceleration Imparted On An Orbiting Planet By a Passingmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Orbital effects of a monochromatic plane gravitational wave with ultra-low frequency incident on a gravitationally bound two-body system

Efroimsky¹

2014

ScienceOpen Research

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“…We recall that, actually, several gravitational waves observatories are planned-and also already operating-to view binaries in various stages of their evolution [26,37], so that they might detect them. For two-body systems effects involving spins linearly, 3 see 4 [17,23,49,76,77].…”

Section: Introductionmentioning

confidence: 99%

General relativistic spin-orbit and spin–spin effects on the motion of rotating particles in an external gravitational field

Iorio

2011

Gen Relativ Gravit

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We analytically compute the orbital effects induced on the motion of a spinning particle geodesically traveling around a central rotating body by the general relativistic two-body spin-spin and spin-orbit leading-order interactions. Concerning the spin-orbit term, we compute the long-term variations due to the particle's spin by finding secular precessions for the inclination I of the particle's orbit, its longitude of the ascending node Ω and the longitude of pericenter . Moreover, we generalize the well-known Lense-Thirring precessions to a generic orientation of the source's angular momentum by obtaining an entirely new effect represented by a secular precession of I , and additional secular precessions of Ω and as well. The spin-spin interaction is responsible of gravitational effects à la Stern-Gerlach consisting of secular precessions of I, Ω, and the mean anomaly M. Such results are obtained without resorting to any approximations either in the particle's eccentricity e or in its inclination I ; moreover, no preferred orientations of both the system's angular momenta are adopted. Their generality allows them to be applied to a variety of astronomical and astrophysical scenarios like, e.g., the Sun and its planets and the double pulsar PSR J0737-3039A/B. It turns out that the orbital precessions caused by the spin-spin and the spin-orbit perturbations due to the less massive body are below the current L. Iorio is a fellow of the Royal Astronomical Society (F. R. A. S.). L. Iorio123 720 L. Iorio measurability level, especially for the solar system and the Stern-Gerlach effects. Concerning the solar Lense-Thirring precessions, the slight misalignment of the solar equator with respect to the ecliptic reduces the gravitomagnetic node precession of Mercury down to a 0.08 mas per century level with respect to the standard value of 1 mas per century obtained by aligning the z axis with the Sun's angular momentum.The new inclination precession is as large as 0.06 mas per century, while the perihelion's rate remains substantially unchanged, amounting to −2 mas per century. Further studies may be devoted to the extrasolar planets which exhibit a rich variety of orbital and rotational configurations.

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General Relativity

2011

Relativistic Celestial Mechanics of the Solar System

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Current status of gravitational wave observations

Cited by 10 publications

References 148 publications

Orbital effects of a monochromatic plane gravitational wave with ultra-low frequency incident on a gravitationally bound two-body system

Orbital effects of a monochromatic plane gravitational wave with ultra-low frequency incident on a gravitationally bound two-body system

General relativistic spin-orbit and spin–spin effects on the motion of rotating particles in an external gravitational field

General Relativity

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