Planetary Flight Handbook. Part 8 - Jupiter swingby missions to Saturn, Uranus, Neptune, and Pluto
Jupiter swingby missions to Saturn, Uranus, Neptune, and Pluto
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Measures of the satellites of Uranus and Mars
Relative measures of satellites of Uranus and Mars from astronomical photographs
Van Biesbroeck, G.↗
Heat protection for atmospheric entry into Saturn, Uranus, and Neptune
Graphitic ablative heat shield fractions and forebody configurations for probe entry into atmospheres of Saturn, Uranus and Neptune
Tauber, M. E.↗
Multicolor photoelectric photometry of Uranus
Narrow band and UBV photoelectric photometry of Uranus geometric albedo and magnitude at unit distance as functions of wavelength
Appleby, J. F.↗
On the methane opacity for Uranus and Neptune.
The contribution of methane to the thermal opacity in the atmospheres of Uranus and Neptune is shown to be negligible. The relevance of this finding lies in the importance of knowing all the sources of thermal opacity to include in models of these atmospheres, for only then may it be possible to deduce their atmospheric structure and composition correctly.
Trafton, L.↗
Limb and polar brightening of Uranus at 8870 A.
Photographs of Uranus in the 8870 A band of methane exhibit limb brightening and brightening at the south pole. The polar brightening is explained by an upper atmospheric haze in addition to Rayleigh scattering by the upper atmosphere. An estimate of the geometric albedo at this wavelength yields a value near 0.01.
Sinton, W. M.↗
The planets Uranus, Neptune, and Pluto (1971)
Design criteria relating to spacecraft intended to investigate the planets of Uranus, Neptune, and Pluto are presented. Assessments were made of the potential effects of environmental properties on vehicle performance. Pertinent data on the mass, radius, shape, mean density, rotational pole location, and mean orbital elements for the three planets are given in graphs and tables.
Palluconi, F. D.↗
Single thrust period missions to Uranus for unmanned nuclear-electric propulsion systems
The effects of trip time, propulsion time, and specific powerplant mass are studied for optimized unmanned probe spacecraft on missions to Uranus with nuclear-electric propulsion systems. Electric propulsion is confined to a single thrust period at the beginning of each mission. Mission profiles include both high-thrust and electric-propulsion Earth-departure modes for planet flyby and orbital capture. Effects of propulsion time and propulsion system parameters are evaluated, and typical design features of the nuclear-electric spacecraft are outlined. Payload capability comparisons are made with systems employing ballistic transfer and solar-electric propulsion.
Zola, C. L.↗
Summary of Saturn swingby missions to Uranus
The interplanetary trajectory characteristics for missions to Uranus, which employ an intermediate swingby of Saturn to reduce the total trip time are summarized. Opportunities for such swingby missions will occur from 1979 through 1987 and not again until 2025. The general trajectory characteristics (C sub 3; departure, swingby, and arrival dates; swingby radius; and arrival speed) are evaluated, and payload and launch window information for a Titan 3E/Centaur/TE-364-4 class launch vehicle is provided.
Manning, L. A.↗
Limb brightening on Uranus - A prediction.
Intensity variation across Uranus disk during limb darkening-brightening cycles observations to test cloud absence theory, predicting limb brightening in methane bands
Belton, M. J. S.↗
The search for HD in the spectrum of Uranus - An upper limit to D/H
An upper limit to the deuterium-to-hydrogen ratio in the atmosphere of Uranus is reported. It is based on the nonobservance of the P(1) line of the 4-0 band of the HD infrared rotation-vibration spectrum. The relation of this limit to measurements reported for the Jovian atmosphere is discussed.
Lutz, B. L.↗
Saturn Uranus atmospheric entry probe mission spacecraft system definition study
The modifications required of the Pioneer F/G spacecraft design for it to deliver an atmospheric entry probe to the planets Saturn and Uranus are investigated. It is concluded that it is feasible to conduct such a mission within the constraints and interfaces defined. The spacecraft required to perform the mission is derived from the Pioneer F/G design, and the modifications required are generally routinely conceived and executed. The entry probe is necessarily a new design, although it draws on the technology of past, present, and imminent programs of planetary atmospheric investigations.
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Uranus science planning
Recommendations for a 1979 Mariner Jupiter-Uranus mission are discussed with the possibility of launching the first outer planet atmospheric entry probe. Measurement categories considered for the mission include conducting imaging experiments, observations in both the IR and UV spectral range, experiments associated with magnetic fields, plasma, charged particles, and S- and X-band occultation measurements.
Moore, J.↗
Effect of initial conditions on deduced atmosphere for Uranus and Jupiter entries
Atmosphere reconstruction based on the data from a probe is discussed in terms of the effect of errors in entry velocity and entry flight path angle on the determination of density, pressure, and temperature as functions of altitude. Emphasis is placed on Uranus and Jupiter entries, although Saturn entries are included.
Kirk, D.↗
Infrared measurements of Uranus and Neptune
New measurements verify that Neptune is brighter than Uranus near 20 microns and show that both planets have increasing brightness temperature with decreasing wavelength between 34 and 22.5 microns. The observations are not compatible with existing models for the atmospheres of these planets.
Rieke, G. H.↗
Observational constraints on model atmospheres for Uranus and Neptune
We have re-examined the visible and near-IR regions of the spectra of Uranus and Neptune to provide additional data for constructing atmospheric models. We find that a true continuum exists only at wavelengths below 4700 A, that the 6420 A absorption previously attributed to hydrogen is probably caused by methane, that there is no evidence for ammonia, ethylene or ethane absorptions in our spectra, and that the abundance of methane is probably much higher than previous estimates suggest. This last finding implies that the value of H/C in the atmospheres of both planets is much less than 1/10 the solar (or Jovian) value. Clear, Rayleigh-scattering model atmospheres are not compatible with the observations, but more work is needed to establish viable alternatives.
Encrenaz, T.↗
Interior structure of Uranus
Critical measurements relative to interior structure which can be made during a spacecraft mission to Uranus are discussed. Models of atmospheric composition, possible magnetic moment, and gravitational harmonics are described, and it is shown that high quality imaging of the atmospheric rotation and determination of the possible magnetic field rotation will facilitate construction of an accurate model of the interior structure of the planet.
Hubbard, W. B.↗