Venus as a more Earth-like planet

  title={Venus as a more Earth-like planet},
  author={H{\aa}kan Svedhem and Dmitry Titov and Fredric W. Taylor and Olivier G. Witasse},
Venus is Earth’s near twin in mass and radius, and our nearest planetary neighbour, yet conditions there are very different in many respects. Its atmosphere, mostly composed of carbon dioxide, has a surface temperature and pressure far higher than those of Earth. Only traces of water are found, although it is likely that there was much more present in the past, possibly forming Earth-like oceans. Here we discuss how the first year of observations by Venus Express brings into focus the… 

Venus: The Atmosphere, Climate, Surface, Interior and Near-Space Environment of an Earth-Like Planet

This is a review of current knowledge about Earth’s nearest planetary neighbour and near twin, Venus. Such knowledge has recently been extended by the European Venus Express and the Japanese Akatsuki

The Outer Edge of the Venus Zone around Main-sequence Stars

A key item of interest for planetary scientists and astronomers is the habitable zone: the distance from a host star where a terrestrial planet can maintain necessary temperatures in order to retain

Accretion and Shifts of the Levels of O 2 and CO 2 in the Biosphere

In the solar system and perhaps beyond, when many aspects are considered, Earth is a unique planet. Often called the twin planet to Earth because of its close proximity, its comparable radius/size,

Presence of water on exomoons orbiting free-floating planets: a case study

A free-floating planet (FFP) is a planetary-mass object that orbits around a non-stellar massive object (e.g. a brown dwarf) or around the Galactic Centre. The presence of exomoons orbiting FFPs has

Universal weather

  • W. Woolf
  • Physics, Environmental Science
  • 2015
ing solar radiation and warms the local atmosphere. This differential heating sets up winds that lift more dust into the air, triggering a positive feedback mechanism, resulting in very large dust

Chapter 14 – Venus: Atmosphere

Can Venus shed microorganisms?

  • G. Konesky
  • Physics, Environmental Science
    Optical Engineering + Applications
  • 2009
The pale featureless cloud tops of Venus reveal a rich complexity when viewed in ultraviolet. These features result from an unknown absorber brought up from lower atmospheric levels by convection,

The electric wind of Venus: A global and persistent “polar wind”‐like ambipolar electric field sufficient for the direct escape of heavy ionospheric ions

Understanding what processes govern atmospheric escape and the loss of planetary water is of paramount importance for understanding how life in the universe can exist. One mechanism thought to be



The loss of ions from Venus through the plasma wake

Measurements of the atmosphere of Venus show that the dominant escaping ions are O+, He+ and H+.

The structure of Venus’ middle atmosphere and ionosphere

The fine structure in temperatures at upper cloud-deck altitudes is determined, a distinct day–night temperature difference in the southern middle atmosphere is detected, and day-to-day changes in Venus’ ionosphere are tracked.

Little or no solar wind enters Venus’ atmosphere at solar minimum

The bow shock under low solar activity conditions seems to be in the position that would be expected from a complete deflection by a magnetized ionosphere, therefore little solar wind enters the Venus ionosphere even at solar minimum.

A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express

Measurements of day-side CO2 non-local thermodynamic equilibrium emission and night-side O2 emission of Venus are reported, which are consistent with three-body recombination of oxygen atoms transported from the day side by a global thermospheric sub-solar to anti-s solar circulation, as previously predicted.

South-polar features on Venus similar to those near the north pole

Observations of Venus’ south-polar region are reported, where clouds with morphology much like those around the north pole, but rotating somewhat faster than the northern dipole are seen.

Morphology and dynamics of the upper cloud layer of Venus

The convective cells in the vicinity of the subsolar point are much smaller than previously inferred, which is interpreted as indicating that they are confined to the upper cloud layer, contrary to previous conclusions, but consistent with more recent study.

A warm layer in Venus' cryosphere and high-altitude measurements of HF, HCl, H2O and HDO

The detection of an extensive layer of warm air at altitudes 90–120 km on the night side of Venus that is interpreted as the result of adiabatic heating during air subsidence is reported.

Lightning on Venus inferred from whistler-mode waves in the ionosphere

Observations of Venus' ionosphere reveal strong, circularly polarized, electromagnetic waves with frequencies near 100 Hz that have the expected properties of whistler-mode signals generated by lightning discharges in Venus’ clouds.