The Hot Atmosphere of Venus might cool the Interior of Earth’s Sister Planet
The heat in the atmosphere of Venus, induced from a strong greenhouse warming, might actually have a cooling effect on the planet's interior. This counter-intuitive theory is based on calculations from a new model presented at the European Planetary Science Congress (EPSC) in Rome on Tuesday 21st September.
"For some decades we’ve known that the large amount of greenhouse gases in the atmosphere of Venus cause the extreme heat we observe presently", explains Lena Noack from the German Aerospace Center (DLR) in Berlin, lead author of the study.
"The carbon dioxide and other greenhouse gases that are responsible for the high temperatures were blown into the atmosphere by thousands of volcanoes in the past. The permanent heat – today we measure almost 470 degrees Celsius globally on Venus – might even have been much higher in the past and, in a runaway cycle, led to even more volcanism. But at a certain point this process turned on its head – the high temperatures caused a partial mobilisation of the Venusian crust, leading to an efficient cooling of the mantle, and the volcanism strongly decreased. This resulted in lower surface temperatures, rather comparable to today's temperature on Venus, and the mobilisation of the surface stopped.”
The source of the magma, or molten rocky material, and the volcanic gases lies deep in the mantle of Venus. The decay of radioactive elements, inherited from the building blocks of the Solar System's planets, and the heat stored in the interior from planet formation produce enough heat to generate partial melts of silicate-, iron- and magnesium-rich magma in the upper mantle. Molten rock has more volume and is lighter than the surrounding solid rock of identical composition. The magma therefore can rise upwards and eventually penetrate through the rigid crust in volcanic vents, spreading lava over the surface and blowing gases into the atmosphere, mostly greenhouse gases like carbon dioxide (CO2), water vapour (H2O) and sulphur dioxide (SO2).
However, the more greenhouse gases, the hotter the atmosphere – possibly leading to even more volcanism. To find out if this runaway process would end in a red-hot Venus, Lena Noack and Doris Breuer, co-author of the study, calculated for the first time a model where the hot atmosphere is 'coupled' to a 3D model of the planet's interior. Unlike here on Earth, the high temperatures have a much bigger effect at the interface with the rocky surface, heating it up to a large extent.
"Interestingly, due to the rising surface temperatures, the surface is mobilised and the insulating effect of the crust diminishes," says Noack. "The mantle of Venus loses much of its thermal energy to the outside. It's a little bit like lifting the lid on the mantle: the interior of Venus suddenly cools very efficiently and the rate of volcanism ceases. Our model shows that after that 'hot' era of volcanism, the slow-down of volcanism leads to a strong decrease of the temperatures in the atmosphere".
The calculations of the geophysicists yield another interesting result: the process of volcanic resurfacing takes place at different places at different times. When the atmosphere cools, the mobilisation of the surface stops. However, there are still a few active volcanoes which resurface some spots with lava flows. Some volcanoes might be active even today, which fits recent results from the European Space Agency’s Venus Express mission. This detected 'hot spots', or unusual high surface temperatures at volcanoes previously thought to be extinct. So far no 'smoking gun', or active volcano has been identified on Venus – but it seems not unlikely that Venus Express or future space probes will detect the first active volcano on Earth's next neighbour.
Temperature distribution within Venus and local mobilization at the surface. Credit: DLR
3-D perspective of the Venusian volcano, Maat Mons generated from radar data from NASA’s Magellan mission.
Venus and Earth: twins in the Solar System with quite different characters
Earth and its inner neighbour Venus are sometimes called 'sister planets' in the solar system: they are about the same size and mass, and both planets orbit in a somewhat comparable distance to the Sun.
However, scientists have been wondering for decades why both planets developed quite differently:
• here, our 'blue marvel' the Earth, has treasure of water harbouring life based. The molecule H2O is very bond-friendly to ions of other atoms or molecules
• there, a hellish Venus has no liquid water at the surface, where it is just too hot. Venus is shrouded with thick, hot and dynamical skies of carbon dioxide where clouds of sulphur acid prevent any glimpse of the surface from outside. It was Venus where we learned how the greenhouse effect works: the solar ray's energy, which is reemitted from the surface, is absorbed by greenhouse gases like CO2, raising the atmosphere's temperature. Though the same process takes place on Earth, it has a much smaller dimension here than on Venus.
The fact that on Venus there is no liquid water present at all shows that something happened differently when these apparent twins formed about 4.5 billion years ago. From radar observations we have a complete survey of the surface features of Venus. They show us that thousands of volcanoes seem to have reshaped most of the surface of the planet, which is in average about 500 million years old.
Paper presented at EPSC
21 September 2010, 14:10, WR1
Coupling of Interior Dynamics Models with Global Atmosphere Models and its Application to Venus. Presented by Lena Noack (DLR Institute of Planetary Research, Berlin, Germany, and Dept. of Planetary Physics, Joint Planetary Interior Physics Research Group of the University Münster, Germany) and Doris Breuer (DLR Institute of Planetary Research)
EUROPEAN PLANETARY SCIENCE CONGRESS (EPSC) 2010
EPSC 2010 is organised by Europlanet, a Research Infrastructure funded under the European Commission’s Framework 7 Programme, in association with the European Geosciences Union, with the support of the Italian National Institute for Astrophysics (INAF) and the INAF Institute of Physics of Interplanetary Space (IFSI) in Rome. EPSC is the major meeting in Europe for planetary scientists. The 2010 programme comprises 48 sessions and workshops covering a wide range of planetary topics.
EPSC 2010 is taking place at the Angelicum Centre – Pontifical University of Saint Thomas Aquinas, Rome, Italy from Sunday 19 September to Friday 24 September 2010.
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For further details, see the meeting website:
EUROPLANET RESEARCH INFRASTRUCTURE (RI)
Europlanet Research RI is a major (€6 million) programme co-funded by the European Union under the Seventh Framework Programme of the European Commission.
Europlanet RI brings together the European planetary science community through a range of Networking Activities, aimed at fostering a culture of cooperation in the field of planetary sciences, Transnational Access Activities, providing European researchers with access to a range of laboratory and field site facilities tailored to the needs of planetary research, as well as on-line access to the available planetary science data, information and software tools, through the Integrated and Distributed Information Service. These programmes are underpinned by Joint Research Activities, which are developing and improving the facilities, models, software tools and services offered by Europlanet
Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR)
in der Helmholtz-Gemeinschaft
Institut für Planetenforschung
12489 Berlin, Germany
From 20-24 September, Dr Noack can be contacted through the EPSC Press Office (see top of release for details)