Response of Doppler spacecraft tracking to gravitational radiation

Estabrook, Frank B.; Wahlquist, H. D.

doi:10.1007/bf00762449

Cited by 332 publications

(344 citation statements)

References 4 publications

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“…If we introduce a set of Cartesian orthogonal coordinates (X, Y, Z) in which the wave is propagating along the Z-axis and (X, Y ) are two orthogonal axes in the plane of the wave (see Figure 3), then the frequency of the laser at time t, ν(t), at the beam splitter of AI B is related to the nominal frequency ν 0 of the laser and the gravitational wave's amplitudes, h + (t) and h × (t), by the following relationship [22,13] …”

Section: The Gravitational Wave Signalmentioning

confidence: 99%

Gravitational wave detection with single-laser atom interferometers

Tinto

2010

Gen Relativ Gravit

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We present a new general design approach of a broad-band detector of gravitational radiation that relies on two atom interferometers separated by a distance L. In this scheme, only one arm and one laser will be used for operating the two atom interferometers. We consider atoms in the atom interferometers not only as perfect inertial reference sensors, but also as highly stable clocks. Atomic coherence is intrinsically stable and can be many orders of magnitude more stable than a laser. The unique one-laser configuration allows us to then apply time-delay interferometry to the responses of the two atom interferometers, thereby canceling the laser phase fluctuations while preserving the gravitational wave signal in the resulting data set. Our approach appears very promising. We plan to investigate further its practicality and detailed sensitivity analysis.

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Section: The Gravitational Wave Signalmentioning

confidence: 99%

Gravitational wave detection with single-laser atom interferometers

Tinto

2010

Gen Relativ Gravit

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“…Gravitational radiation affects the propagation of radio pulses between a pulsar and a telescope at the Earth. The difference between the expected and actual time-of-arrival (TOA) of the pulses -the so-called timing residuals -carries information about the GWs [5][6][7], which can be extracted by correlating the residuals from different pulsar pairs. This type of GW detector is sensitive to radiation in the 10 −9 −10 −7 Hz frequency band, a portion of the spectrum in which a promising class of sources are super-massive black hole binary (SMBHB) systems with masses in the range of ∼ 10 7 − 10 9 M ⊙ during their slow, adiabatic inspiral phase [8][9][10][11][12][13][14].…”

Section: Introductionmentioning

confidence: 99%

Characterizing gravitational wave stochastic background anisotropy with pulsar timing arrays

et al. 2013

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Detecting a stochastic gravitational wave background, particularly radiation from individually unresolvable supermassive black hole binary systems, is one of the primary targets for Pulsar Timing Arrays. Increasingly more stringent upper limits are being set on these signals under the assumption that the background radiation is isotropic. However, some level of anisotropy may be present and the characterisation of the gravitational wave energy density at different angular scales carries important information. We show that the standard analysis for isotropic backgrounds can be generalised in a conceptually straightforward way to the case of generic anisotropic background radiation by decomposing the angular distribution of the gravitational wave energy density on the sky into multipole moments. We introduce the concept of generalised overlap reduction functions which characterise the effect of the anisotropy multipoles on the correlation of the timing residuals from the pulsars timed by a Pulsar Timing Array. In a search for a signal characterised by a generic anisotropy, the generalised overlap reduction functions play the role of the so-called Hellings and Downs curve used for isotropic radiation. We compute the generalised overlap reduction functions for a generic level of anisotropy and Pulsar Timing Array configuration. We also provide an order of magnitude estimate of the level of anisotropy that can be expected in the background generated by super-massive black hole binary systems.

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“…Provided that the wave length of the GW is large compared to the wave length of the light signal, we will use the eikonal or geometrical optics approximation to describe the interaction of the light in gravitational waves. The propagation of the electromagnetic waves in the field of gravitational waves was considered many times and we can refer the reader to several papers dealing with this questions in the geometrical optics approximation [7,21,22,23,24,25]. Our subsequent analysis of this problem will be carried out in close analogy with the paper of Sazhin and Maslova [25], where they have considered the structure of electromagnetic field in Fabry-Perot resonator in the field of gravitational waves.…”

Section: Propagation Of Light Near the Localized Source Of Gravitatiomentioning

confidence: 99%

Detection of gravity waves by phase modulation of the light from a distant star

et al. 2005

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We propose a novel method for detecting gravitational waves (GW), where a light signal emitted from a distant star interacts with a local (also distant) GW source and travels towards the Earth, where it is detected. While traveling in the field of the GW, the light acquires specific phase modulation (which we account in the eikonal approximation). This phase modulation can be considered as a coherent spreading of the given initial photons energy over a set of satellite lines, spaced at the frequency of GW (from quantum point of view it is multi-graviton absorption and emission processes). This coherent state of photons with the energy distributed among the set of equidistant lines, can be analyzed and identified on Earth either by passing the signal through a Fabry-Perot filter or by monitoring the intensity-intensity correlations at different times.

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Response of Doppler spacecraft tracking to gravitational radiation

Cited by 332 publications

References 4 publications

Gravitational wave detection with single-laser atom interferometers

Gravitational wave detection with single-laser atom interferometers

Characterizing gravitational wave stochastic background anisotropy with pulsar timing arrays

Detection of gravity waves by phase modulation of the light from a distant star

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