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      Geophysics From Terrestrial Time-Variable Gravity Measurements : Time-Variable Gravity Measurements

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          Observation of Gravitational Waves from a Binary Black Hole Merger

          On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal. The signal sweeps upwards in frequency from 35 to 250 Hz with a peak gravitational-wave strain of \(1.0 \times 10^{-21}\). It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole. The signal was observed with a matched-filter signal-to-noise ratio of 24 and a false alarm rate estimated to be less than 1 event per 203 000 years, equivalent to a significance greater than 5.1 {\sigma}. The source lies at a luminosity distance of \(410^{+160}_{-180}\) Mpc corresponding to a redshift \(z = 0.09^{+0.03}_{-0.04}\). In the source frame, the initial black hole masses are \(36^{+5}_{-4} M_\odot\) and \(29^{+4}_{-4} M_\odot\), and the final black hole mass is \(62^{+4}_{-4} M_\odot\), with \(3.0^{+0.5}_{-0.5} M_\odot c^2\) radiated in gravitational waves. All uncertainties define 90% credible intervals.These observations demonstrate the existence of binary stellar-mass black hole systems. This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.
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            GRACE measurements of mass variability in the Earth system.

            Monthly gravity field estimates made by the twin Gravity Recovery and Climate Experiment (GRACE) satellites have a geoid height accuracy of 2 to 3 millimeters at a spatial resolution as small as 400 kilometers. The annual cycle in the geoid variations, up to 10 millimeters in some regions, peaked predominantly in the spring and fall seasons. Geoid variations observed over South America that can be largely attributed to surface water and groundwater changes show a clear separation between the large Amazon watershed and the smaller watersheds to the north. Such observations will help hydrologists to connect processes at traditional length scales (tens of kilometers or less) to those at regional and global scales.
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              High-Resolution Surface-Wave Tomography from Ambient Seismic Noise

              Cross-correlation of 1 month of ambient seismic noise recorded at USArray stations in California yields hundreds of short-period surface-wave group-speed measurements on interstation paths. We used these measurements to construct tomographic images of the principal geological units of California, with low-speed anomalies corresponding to the main sedimentary basins and high-speed anomalies corresponding to the igneous cores of the major mountain ranges. This method can improve the resolution and fidelity of crustal images obtained from surface-wave analyses.
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                Author and article information

                Journal
                Reviews of Geophysics
                Rev. Geophys.
                Wiley
                87551209
                December 2017
                December 2017
                November 02 2017
                : 55
                : 4
                : 938-992
                Affiliations
                [1 ]Seismology-Gravimetry; Royal Observatory of Belgium; Uccle Belgium
                [2 ]Littoral, Environnement et Sociétés; Université de La Rochelle and CNRS (UMR7266); La Rochelle France
                [3 ]Geology and Applied Geology Unit, Faculty of Engineering; University of Mons; Mons Belgium
                [4 ]Department of Meteorology and Geophysics; University of Vienna; Vienna Austria
                [5 ]Faculty of Science, Technology and Communication; University of Luxembourg; Esch-sur-Alzette Grand Duchy of Luxembourg
                [6 ]Laboratoire de Volcanologie, G-time, Département Géosciences, Environnement et Société; Université Libre de Bruxelles; Brussels Belgium
                Article
                10.1002/2017RG000566
                52d55850-744d-4596-b0b6-54429e0c8e4d
                © 2017

                http://doi.wiley.com/10.1002/tdm_license_1.1

                http://onlinelibrary.wiley.com/termsAndConditions#vor

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