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… 

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 insertion

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.

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 inner

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.

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.

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 of

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.

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.

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.



The dark side of Venus

  • D. Allen
  • Physics, Environmental Science
  • 1987

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.

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 cloud