Venus Surface Composition Constrained by Observation and Experiment

  title={Venus Surface Composition Constrained by Observation and Experiment},
  author={Martha S. Gilmore and Allan H. Treiman and J. Helbert and Suzanne E. Smrekar},
  journal={Space Science Reviews},
New observations from the Venus Express spacecraft as well as theoretical and experimental investigation of Venus analogue materials have advanced our understanding of the petrology of Venus melts and the mineralogy of rocks on the surface. The VIRTIS instrument aboard Venus Express provided a map of the southern hemisphere of Venus at ∼1 μm allowing, for the first time, the definition of surface units in terms of their 1 μm emissivity and derived mineralogy. Tessera terrain has lower… 

Deriving iron contents from past and future Venus surface spectra with new high-temperature laboratory emissivity data

The new laboratory data show that different rock types can be distinguished using only a small set of spectral bands, and future orbital spectral observations can provide a much-needed global composition map.

Present-day volcanism on Venus as evidenced from weathering rates of olivine

It is shown that olivine becomes coated, within days, with alteration products, primarily hematite (Fe2O3), and the VNIR 1000-nm absorption, characteristic of Olivine, also weakens within days.

Seeing Through the Atmosphere of Venus: What Is on the Surface?

The exploration of the surface geology of Venus has been hampered by its inhospitable conditions and thick and opaque atmosphere. Fundamental properties, such as crustal composition and heterogeneity

The Venus Emissivity Mapper (VEM): obtaining global mineralogy of Venus from orbit

The Venus Emissivity Mapper is the first flight instrument designed with a focus on mapping the surface of Venus using atmospheric windows around 1 μm. After several years of development VEM has a

Numerical modelling of Venus’mantle: the role of cratons in lithospheric overturns

Despite its similarities in bulk properties to Earth, Venus portrays a fundamentally different mode of surface tectonics. Venus is currently known to be operating in stagnant lid mode of mantle

Venus Interior Structure and Dynamics

No two rocky bodies offer a better laboratory for exploring the conditions controlling interior dynamics than Venus and Earth. Their similarities in size, density, distance from the sun, and young



Geochemistry of Venus Basalts with Constraints on Magma Genesis

Introduction: The chemical diversity of planetary basalts has been used to constrain the processes of planetary accretion and evolution; however, without recent mission to Venus to analyze

Petrological modeling of basaltic rocks from Venus: A case for the presence of silicic rocks

The presence of highly evolved igneous rocks on Venus is a controversial issue. The formations of highland terranes and pancake domes are the two principal tectonic and volcanic features which argue

Recent Hotspot Volcanism on Venus from VIRTIS Emissivity Data

Variations in the thermal emissivity of the surface observed by the Visible and Infrared Thermal Imaging Spectrometer on the European Space Agency’s Venus Express spacecraft are used to identify compositional differences in lava flows at three hotspots, indicating that Venus is actively resurfacing.

Mineral equilibria and the high radar reflectivity of Venus mountaintops

We studied the relationship between altitude and microwave emissivity (the complement of power reflectivity) in 10 highland regions of Venus, using the Magellan data set. Above a critical altitude

Tectonic and Thermal Evolution of Venus and the Role of Volatiles : Implications for Understanding the Terrestrial Planets

Venus is similar to Earth in size and bulk composition. The dramatic differences between the two planets indicate that planetary size alone does not control geologic evolution. Earth's geology is

Bell Regio, Venus: Integration of remote sensing data and terrestrial analogs for geologic analysis

The geology and surface morphology of Bell Regio (18–42°N, 32–58°E) are investigated using a combination of Magellan, Venera, and analogous terrestrial data. The properties of surface units are

Venus surface thermal emission at 1 μm in VIRTIS imaging observations: Evidence for variation of crust and mantle differentiation conditions

[1] The Venus Express spacecraft images the nightside thermal emissions using the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS). At 1.02, 1.10, and 1.18 μm, thermal emission from the