Hot Atmosphere of Venus Might Cool the Interior

Article written: 20 Sep , 2010
Updated: 24 Dec , 2015
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Venus is so hot, it’s cool! This very groovy 1960’s-looking image shows the temperature distribution within Venus and local mobilization at the surface, and is the result of new model of the atmosphere of Earth’s sister planet. The model reveals that the heat in the atmosphere induced from a strong greenhouse warming might actually have had a cooling effect on Venus’ interior. While counter intuitive, the theory might explain why Venus was a highly volcanic planet in the past. And interestingly, it might mean that Venus may have some active volcanoes even today. If so, that would be like, outta sight, man!

“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,” said Lena Noack from the German Aerospace Center (DLR) in Berlin, lead author of the study who presented her findings at the European Planetary Science Congress (EPSC) in Rome.

“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, “ Noack said. “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 mobilization of the Venusians 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 mobilization 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 vapor (H2O) and sulfur dioxide (SO2).

3-D perspective of the Venusian volcano, Maat Mons generated from radar data from NASA’s Magellan mission.

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 mobilized and the insulating effect of the crust diminishes,” said 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 mobilization of the surface stops. However, there are indications from the European Space Agency’s Venus Express mission that there may be a few active volcanoes even today which resurface some spots with lava flows. While no volcanic activity has acutally been seen, Venus Express has 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 perhaps Venus Express or future space probes will detect the first active volcano on Earth’s neighbor.

Source: European Planetary Science Conference



3 Responses

  1. Uncle Fred says

    Not sure if I get this one. Why is the heat transfer from the interior to the crust different to Earth’s? Does this have something to do with Earth’s plate tectonics and Venus’s lack thereof?

  2. Torbjorn Larsson OM says

    Fred, good guess.

    A large terrestrial (i.e Earth-like) differentiated (i.e. having core) planet looses its core heat, which it gained by gravitational and radioactive energy conversion, over geological times. This happens naturally through gravitational convection in the highly viscous slowly moving mantle.

    The solid crust acts as an insulating lid that bounds and partly defines the mantle convection. So either you have plate tectonics that recirculates the core to let heat out, or it is suspected you have partial or total episodic crust melting.

    The difference is believed to lie in having seas, which enables crust recycling through a) making the crust malleable, b) easier to melt, and c) enables magmas and recycled crust to tend to granitic balance. Granites are rock eutectics, i.e. crystallizes first, and gives a well defined dynamic steady state for plate tectonic rock.

    Venus hot-house have somehow lost its water, likely to space through hydrogen and atomic oxygen loss, so no plate tectonics. Interesting point IMHO is that the research seems to find partial melting through their atmospheric back reaction, which confirm the finds of different and putative older geological formations.

    That could also mean that one can reach back in geological history. Perhaps back to the time when twin planets Earth and Venus diverged in geological and atmospheric paths.

    Another touch point is those hot spots. If they are analogous to either Earth magmatic pockets or our own “hot spots” that makes volcano chain geology such as Hawaii or Iceland, it can help understanding there. I’m not a geologist, but it seems to me from the small amount what I read on those that either process is less well understood.

    Finally, I wonder if the radical change in some or all of the atmosphere (“a strong decrease of the temperatures in the atmosphere””) somehow translates to varying atmospheric loss rates during Venus history. That would be both cumbersome to riddle and interesting in the context.

    Venus has gone from simple to “you magnificent bastard”.

  3. Uncle Fred says

    Okay. Thanks for the explanation OM.

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