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Terraforming is the process of changing the global environment of a planet  in such a way as to make it suitable for human habitation. Because it is so far beyond our current technological capabilities, most articles about terraforming have been written by science fiction writers rather than scientists.  For example, there is  an entry for a terraformed Venus in the science fiction work “Encyclopaedia Galactica” which is set thousands of years in the future.

Originally a hot dry greenhouse world, (Cytherian Type) with an atmosphere consisting mostly of carbon dioxide with a surface pressure 94 times greater than that of Earth. The planet was shrouded with clouds of sulphuric and hydrochloric acid and the mean surface temperature was 480 C, making the world extremely hostile to terragen and carbon-based life. Because of this the planet was sparsely populated for many thousands of years; recently it has been successfully terraformed.

(Kazlev et al 2006).

Even though I know of very few references to a terraformed Venus in serious scientific writing, there is no reason why – given sufficient resources and time – an advanced human civilisation wouldn’t be able to terraform Venus. In this post I’ll talk about the challenges to making Venus habitable so that humans can live and work on the planet without any need for protective equipment such as space suits or oxygen supplies.


What a terraformed Venus might look like – Image from Wikimedia Commons

High Temperatures and Pressures.

The surface temperature of Venus is around 500 degrees Celsius and the atmospheric pressure is a crushing  92 times that of the Earth. The atmosphere consists of 97%  carbon dioxide (Williams 2015), a powerful greenhouse gas which traps the Sun’s heat. In order to make the planet habitable the surface temperature would need to be around 0 to 35 degrees and the atmospheric pressure similar to that on the Earth.

One way to cool Venus would be to build a giant sunshade to block most of the Sun’s rays from hitting the planet. This was described in detail in a paper written by the late British science writer Paul Birch (1991).

Venus Sunshade

The shade would orbit the Sun at a specific point about 1 million km above the planet’s surface called the L1 Lagrange point, shown as L in the diagram above (see note 1). It would need to be slightly larger than the diameter of Venus, 12,100 km, to fully shade the planet. The cost and technological challenge of building such a shade would enormous. It would need to be 100 billion times larger in surface area than the International Space station, shown below, which is the largest object ever built in space.


It is likely that such a shade would be built up from thousands or even millions of smaller individual shades and would take many decades to complete from start to finish. As the shade neared completion, and most of the Sun’s rays were blocked from hitting the planet, the surface of Venus would begin to cool.  Interestingly, when the shade was complete, because Venus would no longer be lit up by the Sun, to an observer on Earth Venus would go from being the third brightest object in the sky (after the Sun and the Moon) to being invisible.

After about 100 years the temperature of Venus would drop to 31 degrees (see note 2). At this temperature, known as the critical point of carbon dioxide, some of the carbon dioxide in the atmosphere would start to condense from gas to liquid and the low-lying areas of the surface of Venus would begin to be covered in seas and oceans of liquid carbon dioxide, in the same way that much of the Earth’s surface is covered by seas and oceans of water. As it condensed into liquid, the amount of carbon dioxide left in the atmosphere would start to fall and with it the atmospheric pressure.

Eventually the temperature would drop to the freezing point of carbon dioxide (-57 degrees) and the seas, oceans and lakes of liquid carbon dioxide would begin to freeze. Much of the remaining carbon dioxide in the atmosphere would fall as snow.

This entire cooling process would take hundreds of years from start to finish. When it had completed the next step would be to ensure that when the shade was removed, allowing the planet to warm up, the frozen carbon dioxide wasn’t released back into the atmosphere. One way this could be achieved would be to cover up the frozen carbon dioxide oceans with an insulating material and provide some sort of refrigeration system to keep it cool. Once the carbon dioxide was safely locked away the sunshade could then be removed to allow the planet to warm up again. Because nearly all the carbon dioxide would have been removed from the atmosphere it would no longer provide such a powerful greenhouse gas.

No Water

Venus is a very dry planet. Its atmosphere contains only a small trace of water and there is no water on its surface. By comparison, on Earth 71% of the planet’s surface is covered by water and  there are about 1.39 billion cubic kilometers of water on the planet.  The breakdown of how this water is distributed is shown in the tables below (U.S. Department of the Interior 2015)

Earth Water

As water is essential for life, it would be necessary to import water to Venus to make the entire planet habitable for plant and animal life. A lot of water would be needed, but it would not be necessary to have most of the planet covered with deep oceans of water. Probably around 30-50 million cubic kilometres of water would be sufficient. Even so, this is a still a huge amount of water to shift.

How could we get a large amount of water to Venus?

There various ways of doing this. One way would be to transport it from the seas and oceans of Earth. The cost of this would we be prohibitive and even if there are huge advances in technology it would be extremely difficult to transport a huge amount of water by this method.

Another possibility, again prohibitively expensive, would be to import hydrogen by scooping it up on an orbiting ring from one of the giant planets in the outer Solar System. The hydrogen would then be sent onto Venus by a cargo-carrying spacecraft. The hydrogen would produce water by chemical reaction with the remaining carbon dioxide in the planet’s atmosphere.

A fascinating alternative way of getting all the water needed to Venus was suggested in Birch’s paper.  It involves moving one of Saturn’s ice moons into orbit around Venus and then breaking it up, thus releasing all the water needed onto the planet.

Saturn has a number of ice moons such as Hyperion (shown below), an irregularly shaped object 360 by 260 km which consist mainly of ice, covered in a thin layer of rock.


Image from NASA

The proposal is that we could build a huge structure on Hyperion which would use the Sun’s heat, concentrated by mirrors, to put out a jet of steam into space in the same direction as it orbits Saturn. This is shown in the diagram below.

Hyperion Steam Engine


This jet of steam will provide a force which will gradually slow down Hyperion in its orbit causing it to gradually spiral inwards towards Saturn. After about 30 years Hyperion will be in an oval-shaped orbit which will cause it to pass close to the giant moon Titan.

Hyperion Steam Orbit Decay

Titan is much larger than Hyperion and the near collision between the two objects will give Hyperion so much speed that it will be ejected from orbit around Saturn.  If the speed and angle are just right, after it escapes from Saturn it will be on a path which will take it close to the giant planet Jupiter. This technique is known as a slingshot and NASA uses it to send spacecraft to the outer Solar System.

As Hyperion passes Jupiter, the giant planet’s gravity will hurl it into the inner Solar System. If the angle of approach to Jupiter is just right it will be possible to send it on such a path that it will approach Venus slowly enough to be captured by Venus’s gravity and go into orbit around the planet. Once in orbit Hyperion would be gradually broken up and its water transferred to the planet’s surface.

Although this somewhat convoluted plan might appear to be something out of an exotic science fiction story, it obeys all the laws of physics and could potentially be achieved by an advanced human civilisation which devoted the resources to do it.

No oxygen

In order to be habitable Venus would need a similar level of oxygen in its atmosphere to that on the Earth. On Earth oxygen makes up about 21% of the atmosphere, whereas Venus’s atmosphere has almost no oxygen.  Compared to the other challenges this would be relatively easy to resolve. The oxygen concentration could be increased by plant life which, as you may remember from your high school biology lessons, uses a process called photosynthesis to convert carbon dioxide and water into carbohydrates and oxygen.


Image from Wikimedia Commons

Long day/night cycle

On Venus the slow rotation of the planet means that a day lasts 116.8 Earth days. Most Earth lifeforms would struggle to adapt to such a long day/night cycle. A shorter day could be created by means of orbiting shades and mirrors.

No magnetic field

On the Earth its magnetic field forms a protective shield around the planet which protects its surface from electrically charged particles from the Sun (the solar wind) and from outer space (cosmic rays). Without a magnetic field  there would be an increased risk of cancer for anyone who ventured outdoors for any significant period of time.  To make Venus completely habitable it would need to be given an artificial magnetic field. This is actually quite difficult to do, even for an advanced civilisation, and will merit its own blog post in due course!


The Science Geek



1) At this point the shade would orbit the Sun in exactly the same time, 224.7 days, that it takes Venus to orbit the Sun. Therefore it would always be shading the planet once it was put in place.

2) Any timescales here should be treated as very approximate. The actual values depend on the properties of the Venusian atmosphere during the cooling scenario.


Birch, P. (1991) Terraforming Venus quickly, Available at:http://www.orionsarm.com/fm_store/TerraformingVenusQuickly.pdf (Accessed: 6 February 2016).

Kazlev, M.A., Sandberg M., Bowers, S., Parisi M (2006) Encyclopaedia Galactica -Venus, Available at: http://www.orionsarm.com/eg-article/48e7ce77477af (Accessed: 11th February 2016).

U.S. Department of the Interior (2015) How much water is there on, in, and above the Earth?, Available at: http://water.usgs.gov/edu/earthhowmuch.html (Accessed: 7 February 2016).

Williams D R (2015) Venus fact sheet, Available at:http://nssdc.gsfc.nasa.gov/planetary/factsheet/venusfact.html (Accessed: 6 February 2016).