The Voyager Ultraviolet Spectrometer (UVS) is an objective grating spectrometer covering the wavelength range of 500–1700 A with 10 A resolution. Its primary goal is the determination of the composition and structure of the atmospheres of Jupiter, Saturn, Uranus and several of their satellites. The capability for two very different observational modes have been combined in a single instrument. Observations in the airglow mode measure radiation from the atmosphere due to resonant scattering of the solar flux or energetic particle bombardment, and the occultation mode provides measurements of the atmospheric extinction of solar or stellar radiation as the spacecraft enters the shadow zone behind the target. In addition to the primary goal of the solar system atmospheric measurements, the UVS is expected to make valuable contributions to stellar astronomy at wavelengths below 1000 A.

http://deepblue.lib.umich.edu/bitstream/handle/2027.42/43773/11214_2004_Article_BF00200850.pdf?sequence=1

Ultraviolet spectrometer experiment for the Voyager mission

Phase-retrieval measurements of point-spread functions from the pre- and post-repair Hubble Space Telescope are presented. The primary goal was to determine the aberrations present in the second wide-field and planetary camera (WFPC2) to align and validate its corrective optics. With both parametric model-fitting techniques and iterative (Gerchberg-Saxton) methods, accurate measurements have been obtained of the WFPC2 and Hubble Space Telescope optics, including improved maps of the zonal errors in the mirrors. Additional phase-retrieval results were obtained for the aberrated, prerepair cameras and the corrected faint-object camera. The information has been used to improve models produced by point-spread-function simulation programs. On the basis of the measurements a conic constant for the primary mirror of κ = -1.0144 has been derived.

Phase-retrieval analysis of pre- and post-repair Hubble Space Telescope images.

A survey of current knowledge about Jupiter, Saturn, Uranus, Neptune, Pluto, and their satellites is presented. The best available numerical values are given for physical parameters, including orbital and body properties, atmospheric composition and structure, and photometric parameters. The more acceptable current theories of these bodies are outlined with thorough referencing offering access to the details. The survey attempts to cover the literature through May 1, 1972.

A survey of the outer planets Jupiter, Saturn, Uranus, Neptune, Pluto, and their satellites

Physical and chemical processes which affect the equilibrium distribution of ionization in the atmospheres of Jupiter, Saturn, Uranus and Neptune are reviewed. Current models imply readily detectable ionospheres for all four planets and suggest that protons should represent the dominant positive ion. Attention is directed to the probable importance of dissociative ionization of H2 as a source of H+. A number of potentially important loss mechanisms for H+ are discussed including a possible reaction of H+ with vibrationally excited H2. Protons may be removed efficiently at lower altitudes by reaction with CH4 and this process may offer a simple remote means for location of the turbopause.

The ionospheres of the major planets

We review here observations and models related to the chemical and thermal structures, airglow and auroral emissions and dynamics of the Venus thermosphere, and compare empirical models of the neutral densities based in large part on in situ measurements obtained by the Pioneer Venus spacecraft. Observations of the intensities of emissions are important as a diagnostic tool for understanding the chemical and physical processes taking place in the Venus thermosphere. Measurements, ground-based and from rockets, satellites, and spacecraft, and model predictions of atomic, molecular and ionic emissions, are presented and the most important sources are elucidated. Coronas of hot hydrogen and hot oxygen have been observed to surround the terrestrial planets. We discuss the observations of and production mechanisms for the extended exospheres and models for the escape of lighter species from the atmosphere. Over the last decade and a half, models have attempted to explain the unexpectedly cold temperatures in the Venus thermosphere; recently considerable progress has been made, although some controversies remain. We review the history of these models and discuss the heating and cooling mechanisms that are presently considered to be the most important in determining the thermal structure. Finally, we discuss major aspects of the circulation and dynamics of the thermosphere: the sub-solar to anti-solar circulation, superrotation, and turbulent processes.

Structure, Luminosity, and Dynamics of the Venus Thermosphere

Rocket Measurement of Ultraviolet Spectra of Venus and Jupiter Between 1200 and 1800 Å

Venus and Jupiter low resolution UV spectra obtained with servocontrolled star tracking telescope in Aerobee rocket, noting Lyman alpha radiation characteristics

Rocket measurement of ultraviolet spectra of Venus and Jupiter between 1200 and 1800 angstrom units.

Reflective correctors to compensate the spherical aberration in the Hubble Space Telescope are placed in front of three of the axial scientific instruments (a camera and two spectrographs) during the first scheduled refurbishment mission. The five correctors required are deployed from a new module that replaces the fourth axial instrument. Each corrector consists of a field mirror and an aspherical, aberration-correcting reimaging mirror. In the camera the angular resolution capability is restored, be it in reduced fields, and in the spectrographs the potential for observations in crowded areas is regained along with effective light collection at the slits.

Reflective correctors for the Hubble Space Telescope axial instruments.

Rocket telescope spectrometer precision pointing achieved by servocontrolling secondary mirror, discussing use for planetary atmospheres far UV spectrum studies

A Rocket Telescope Spectrometer with High Precision Pointing Control

Far UV spectral intensity of B3 V star from Aerobee rocket scanning prism spectrometry, noting discrepancy with model atmosphere predictions

M. Bottema

Papers

Rocket Measurement of Ultraviolet Spectra of Venus and Jupiter Between 1200 and 1800 Å

Rocket measurement of ultraviolet spectra of Venus and Jupiter between 1200 and 1800 angstrom units.

Reflective correctors for the Hubble Space Telescope axial instruments.

A Rocket Telescope Spectrometer with High Precision Pointing Control

The far-ultraviolet spectral intensity of a B3 V star.