The Galileo Venus Encounter

  title={The Galileo Venus Encounter},
  author={Torrence V. Johnson and C. M. Yeates and Richard E. Young and J. Dunne},
  pages={1516 - 1518}
The Galileo spacecraft passed Venus on its way to Jupiter on 10 February 1990, less than 4 months after launch from Earth aboard the shuttle Atlantis. Because Galileo's instruments were selected for broad-based planetary exploration, the spacecraft was able to obtain a wide range of measurements during the Venus encounter. Together with ground-based observations conducted during the encounter, these observations have yielded more accurate information about the planet's plasma environment, cloud… Expand
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Overview of Venus orbiter, Akatsuki
The Akatsuki spacecraft of Japan was launched on May 21, 2010. The spacecraft planned to enter a Venus-encircling near-equatorial orbit in December 7, 2010; however, the Venus orbit insertionExpand
Plasma Observations at Venus with Galileo
Solar wind densities and bulk speeds were determined from the electron velocity distributions, and a search for pickup ions from the hot hydrogen and oxygen planetary coronas yielded an upper limit in the range of 10-3 ion per cubic centimeter, which is consistent with densities expected from current models of neutral gas densities. Expand
Serendipitous science from flybys of secondary targets: Galileo at Venus, Earth, and asteroids; Ulysses at Jupiter
During this quadrennium, while the Voyager and Pioneer spacecraft moved through the outer heliosphere, ever further from the sun, the Ulysses and Galileo spacecraft were traversing the innerExpand
Energetic Particles at Venus: Galileo Results
Comparisons with model bow shock calculations show that shock-drift acceleration in the venusian bow shock seems the most likely process responsible for the observed ions. Expand
Images from Galileo of the Venus Cloud Deck
Images of Venus taken at 418 (violet) and 986 (NIR) nanometers show that the morphology and motions of large-scale features change with depth in the cloud deck, and the zonal flow field shows a longitudinal periodicity that may be coupled to the formation ofLarge-scale planetary waves. Expand
Clouds and Hazes of Venus
More than three decades have passed since the publication of the last review of the Venus clouds and hazes. The paper published in 1983 in the Venus book summarized the discoveries and findings ofExpand
A Global Traveling Wave on Venus
A detailed calculation of linear wave modes in the Venus atmosphere verifies that the dominant large-scale pattern in the clouds of Venus has been described as a "γ" or "Ψ" and tentative identified as a Kelvin wave. Expand
A correlated-k model of radiative transfer in the near-infrared windows of Venus
Abstract We present a correlated- k -based model for generating synthetic spectra in the near-infrared window regions, from 1.0 to 2.5 μm, emitted from the deep atmosphere of Venus on the nightside.Expand
Overview of Venus orbiter ,
M. Nakamura1, T. Imamura1, N. Ishii1, T. Abe1, T. Satoh1, M. Suzuki1, M. Ueno1, A. Yamazaki1, N. Iwagami2, S. Watanabe3, M. Taguchi4, T. Fukuhara3, Y. Takahashi3, M. Yamada1, N. Hoshino5, S.Expand
Transient immunosuppression allows transgene expression following readministration of adeno-associated viral vectors.
It is demonstrated that readministration of rAAV can be accomplished by down regulating the anti-AAV immune response and the use of repeated administration of r AAV as a viable form of therapy for the treatment of chronic diseases is suggested. Expand


The dark side of Venus
Abstract Ground-based infrared observations have been made of the night hemisphere of the planet Venus around 1.7 and 2.3 μm, confirming the continued presence of dark and light patterns at theseExpand
The Nature of the Near-Infrared Features on the Venus Night Side
Near-infrared images of the Venus night side show bright contrast features that move from east to west, in the direction of the cloud-top atmospheric superrotation, which indicates that there are partial clearings in this cloud deck. Expand
Cloud structure on the dark side of Venus
Observations of the dark side of the planet Venus at infrared wavelengths between 1.5 and 2.5 µm have shown it to be anomalously bright in portions of this waveband, and to exhibit structured cloudExpand