Deep space network enhancement for the Galileo mission to Jupiter

Peng, T. K.; Armstrong, J. W.; Breidenthal, Julian C.; Donivan, F. F.; Ham, N. C.

doi:10.1016/0094-5765(88)90041-0

Cited by 5 publications

(3 citation statements)

References 11 publications

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“…Analyses of the noises affecting high-sensitivity Doppler experiments have been published, for example, by Wahlquist et al [1977], Estabrook [1978], Peng et al [1988], Armstrong [1989], and Riley et al [1990]. The noise sources usually considered are propagation noise (tropospheric and plasma scintillation), ground electronics noise (frequency standard and frequency distribution, transmitter, and receiver), antenna mechanical noise, thermal noise, and spacecraft noise (electronics and unmodeled motion of the spacecraft).…”

Section: Transfer Functionsmentioning

confidence: 99%

“…The tracking stations have been designed for excellent instrumental frequency stability, and the electronics were referenced to hydrogen-maser frequency standards; the result was very low phase noise from the instrumentation [Peng et al, 1988]. For Me and MGS the received predetection electric field was downconverted to baseband, sampled using the Radio Science Subsystem [Asmar and Renzetti, 1993], and the signal phase and.…”

Section: Observationsmentioning

confidence: 99%

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Radio wave phase scintillation and precision Doppler tracking of spacecraft

Armstrong¹

1998

Radio Science

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Abstract. Phase scintillation caused by propagation through solar wind, ionospheric, and tropospheric irregularities is a noise process for many spacecraft radio science experiments. In precision Doppler tracking observations, scintillation can be the dominant noise process. Scintillation statistics are necessary for experiment planning and in design of signal processing procedures. Here high-precision tracking data taken with operational spacecraft (Mars Observer, Galileo, and Mars Global Surveyor) and ground systems are used to produce temporal statistics of tropospheric and plasma phase scintillation. The variance of Doppler frequency fluctuations is approximately decomposed into two propagation processes. The first, associated with distributed scattering along the sight line in the solar wind, has a smooth spectrum. The second, associated principally with localized tropospheric scattering for X-band experiments, has a marked autocorrelation peak at the two-way light time between the Earth and the spacecraft (thus a cosine-squared modulation of the fluctuation power spectrum). For X-band data taken in the antisolar hemisphere the average noise levels of this process are in good agreement with average tropospheric noise levels determined independently from water vapor radiometer observations and radio interferometic data. The variance of the process having a smooth spectrum is consistent with plasma noise levels determined independently from dualfrequency observations of the Viking spacecraft made at comparable Sun-Earth-spacecraft angles. The observations reported here are used to refine the propagation noise model for Doppler tracking of deep space probes. In particular, they can be used to predict propagation noise levels for high-precision X-and Ka-band tracking observations (e.g., atmosphere/ionosphere/ring occultations, celestial mechanics experiments, and gravitational wave experiments) to be done using the Cassini spacecraft.

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Section: Transfer Functionsmentioning

confidence: 99%

Section: Observationsmentioning

confidence: 99%

Radio wave phase scintillation and precision Doppler tracking of spacecraft

Armstrong¹

1998

Radio Science

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“…However, in the two-way method described above the measurement suffers inevitably from two main technical limits. Firstly, in frequency changes of the Doppler response, the noise such as the Earth troposphere, ionosphere and the mechanical vibrations of the ground station comprises a major part in the Doppler signal [21,22]. With this, a two one-way measurement method was put forward to cancel the ground-based noise, via mathematically combining the individual Doppler response measured on board the spacecraft and on ground [23][24][25].…”

Section: Introductionmentioning

confidence: 99%

Low-frequency gravitational wave detection via double optical clocks in space

Wang

Wang³

et al. 2018

Class. Quantum Grav.

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We propose a Doppler tracking system for gravitational wave detection via Double Optical Clocks in Space (DOCS). In this configuration two spacecrafts (each containing an optical clock) are launched to space for Doppler shift observations. Compared to the similar attempt of gravitational wave detection in the Cassini mission, the radio signal of DOCS that contains the relative frequency changes avoids completely noise effects due for instance to troposphere, ionosphere, ground-based antenna and transponder. Given the high stabilities of the two optical clocks (Allan deviation ∼ 4.1 × 10 −17 @ 1000 s), an overall estimated sensitivity of 5 × 10 −19 could be achieved with an observation time of 2 years, and would allow to detect gravitational waves in the frequency range from ∼ 10 −4 Hz to ∼ 10 −2 Hz.

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