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The gravitational wave experimentSince the optimum size of a gravitational wave detector is the wave length, interplanetary dimensions are needed for the mHz band of interest. Doppler tracking of Ulysses will provide the most sensitive attempt to date at the detection of gravitational waves in the low frequency band. The driving noise source is the fluctuations in the refractive index of interplanetary plasma. This dictates the timing of the experiment to be near solar opposition and sets the target accuracy for the fractional frequency change at 3.0 x 10 exp -14 for integration times of the order of 1000 sec. The instrumentation utilized by the experiment is distributed between the radio systems on the spacecraft and the seven participating ground stations of the Deep Space Network and Medicina. Preliminary analysis is available of the measurements taken during the Ulysses first opposition test.
Document ID
19920041696
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Bertotti, B.
(Pavia, Universita Italy)
Ambrosini, R.
(CNR Istituto di Radioastronomia, Bologna, Italy)
Asmar, S. W.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA, United States)
Brenkle, J. P.
(JPL Pasadena, CA, United States)
Comoretto, G.
(Arcetri Osservatorio Astrofisico, Florence, Italy)
Giampieri, G.
(Pavia, Universita Italy)
Less, L.
(Jet Propulsion Lab., California Inst. of Tech. Pasadena, CA, United States)
Messeri, A.
(CNR Istituto di Fisica dello Spazio Interplanetario, Frascati, Italy)
Wahlquist, H. D.
(JPL Pasadena, CA, United States)
Date Acquired
August 15, 2013
Publication Date
January 1, 1992
Publication Information
Publication: Astronomy and Astrophysics Supplement Series
Volume: 92
Issue: 2, Ja
ISSN: 0365-0138
Subject Category
Space Sciences (General)
Accession Number
92A24320
Distribution Limits
Public
Copyright
Other

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