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By Y. Choquet-Bauhat, et al.,

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Page breaks are true to the original; line lengths, word breaks, heading styles, and other typesetting-specific formatting, however, cannot be retained, and some typographic errors may have been accidentally inserted. Please use the print version of this publication as the authoritative version for attribution. SEARCH FOR GRAVITATIONAL WAVES: INTRODUCTION 38 SOURCES Because of the weakness of the gravitational interaction, it seems impossible to create on Earth a source of gravitational waves strong enough to be sensed by any conceivable detector; this means that it is impossible to carry out the gravitational analog of Hertz's experiment, and we must depend on cosmic sources to excite detectors.

The uncertainty in the determination of the total perihelion advance decreases as the `3/2 power of the time interval spanned by the data, so a long-term program is important. Given the current infrequency of planetary spacecraft missions (see below), it is particularly important to maintain and improve our radar capability. Sustained high-accuracy measurements of the echo delay of radar signals between the Earth and the inner planets are being accomplished at present with the NASA-supported radar facilities at the Arecibo Observatory and at the Goldstone Tracking Station.

Laser range measurements are routinely made to three widely separated arrays. No degradation of their optical reflectivity has been observed. 2) have been made for over a decade with an uncertainty of about 10 cm from 20 minutes of observation. Recently, additional sites in Hawaii and Australia have joined the McDonald Observatory in Texas and the Grasse Observatory in France in making regular range measurements. The accuracy from the new stations and, after improvements, from the older stations is expected to be a few cm.

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Analysis, Manifolds and Physics [Part 2] by Y. Choquet-Bauhat, et al.,


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