A xylophone detector in space

Massimo Tinto

Banach Center Publications (1997)

  • Volume: 41, Issue: 2, page 155-162
  • ISSN: 0137-6934

Abstract

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We discuss spacecraft Doppler tracking for detecting gravitational waves in which Doppler data recorded on the ground are linearly combined with Doppler measurements made on board a spacecraft. By using the four-link radio system first proposed by Vessot and Levine [1] we derive a new method for removing from the combined data the frequency fluctuations due to the Earth troposphere, ionosphere, and mechanical vibrations of the antenna on the ground. This method also reduces the frequency fluctuations of the clock on board the spacecraft by several orders of magnitude at selected Fourier components, making Doppler tracking the equivalent of a xylophone detector of gravitational radiation [2]. In the assumption of calibrating the frequency fluctuations induced by the interplanetary plasma, a strain sensitivity equal to 4 . 7 × 10 - 18 at 10 - 3 Hz is estimated. This experimental technique could be extended to other tests of the theory of relativity, and to radio science experiments that rely on high-precision Doppler measurements.

How to cite

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Tinto, Massimo. "A xylophone detector in space." Banach Center Publications 41.2 (1997): 155-162. <http://eudml.org/doc/252229>.

@article{Tinto1997,
abstract = {We discuss spacecraft Doppler tracking for detecting gravitational waves in which Doppler data recorded on the ground are linearly combined with Doppler measurements made on board a spacecraft. By using the four-link radio system first proposed by Vessot and Levine [1] we derive a new method for removing from the combined data the frequency fluctuations due to the Earth troposphere, ionosphere, and mechanical vibrations of the antenna on the ground. This method also reduces the frequency fluctuations of the clock on board the spacecraft by several orders of magnitude at selected Fourier components, making Doppler tracking the equivalent of a xylophone detector of gravitational radiation [2]. In the assumption of calibrating the frequency fluctuations induced by the interplanetary plasma, a strain sensitivity equal to $4.7 × 10^\{-18\}$ at $10^\{-3\}$ Hz is estimated. This experimental technique could be extended to other tests of the theory of relativity, and to radio science experiments that rely on high-precision Doppler measurements.},
author = {Tinto, Massimo},
journal = {Banach Center Publications},
keywords = {spacecraft Doppler tracking; detecting gravitational waves},
language = {eng},
number = {2},
pages = {155-162},
title = {A xylophone detector in space},
url = {http://eudml.org/doc/252229},
volume = {41},
year = {1997},
}

TY - JOUR
AU - Tinto, Massimo
TI - A xylophone detector in space
JO - Banach Center Publications
PY - 1997
VL - 41
IS - 2
SP - 155
EP - 162
AB - We discuss spacecraft Doppler tracking for detecting gravitational waves in which Doppler data recorded on the ground are linearly combined with Doppler measurements made on board a spacecraft. By using the four-link radio system first proposed by Vessot and Levine [1] we derive a new method for removing from the combined data the frequency fluctuations due to the Earth troposphere, ionosphere, and mechanical vibrations of the antenna on the ground. This method also reduces the frequency fluctuations of the clock on board the spacecraft by several orders of magnitude at selected Fourier components, making Doppler tracking the equivalent of a xylophone detector of gravitational radiation [2]. In the assumption of calibrating the frequency fluctuations induced by the interplanetary plasma, a strain sensitivity equal to $4.7 × 10^{-18}$ at $10^{-3}$ Hz is estimated. This experimental technique could be extended to other tests of the theory of relativity, and to radio science experiments that rely on high-precision Doppler measurements.
LA - eng
KW - spacecraft Doppler tracking; detecting gravitational waves
UR - http://eudml.org/doc/252229
ER -

References

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  1. [1] R. F. C. Vessot and M. W. Levine, Gen. Relativ. Gravit. 10, 181 (1979). 
  2. [2] M. Tinto, Phys. Rev. D. May 15, 1996. 
  3. [3] J. D. Anderson et al., Science, 207, pp. 449-453,1980. 
  4. [4] J. D. Anderson et al., Icarus, 71, pp. 337-349, 1986. 
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  6. [6] J. W. Armstrong, R. Woo and F. B. Estabrook, Ap. J. , 30 574, 1979. 
  7. [7] I. I. Shapiro et al., Journal of Geophysical Research, 82, pp. 4329-4334, 1977. 
  8. [8] J. D. Anderson et al., Astronautica, 5, pp. 43-61, 1978. 
  9. [9] J. W. Armstrong, In: Gravitational Wave Data Analysis, ed. Schutz, B. F., p. 153 (1989), (Dordrecht, Kluwer). 
  10. [10] L. L. Smarr, R. F. C. Vessot, C. A. Lundquist, R. Decher, and T. Piran, Gen. Relativ. Gravit. 15, 2 (1983). 
  11. [11] A. L. Riley, D. Antsos, J. W. Armstrong, P. Kinman, H. D. Wahlquist, B. Ber- totti, G. Comoretto, B. Pernice, G. Carnicella, and R. Giordani, Jet Propulsion Laboratory Report, Pasadena, California, January 22, (1990). 
  12. [12] LISA: Laser Interferometer Space Antenna for the detection and observation of gravitational waves. A Cornerstone Project in ESA's long term space science program Horizon 2000 Plus, Pre-Phase A Report, MPQ 208, (December 1995). 

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