Some say that Venus could be a better option for terraforming than Mars. However, the planetary community is not in favor of terraforming anything. 

Here are some proposed approaches to terraforming Venus:

• Eliminate the atmosphere 
• Cool the planet with solar shades 
• Combine solar shades and atmospheric condensation 
• Place a planet-sized reflector between Venus and the Sun 
• Deal with the 465 quadrillion metric tons of carbon dioxide The main problem with Venus is its thick carbon dioxide atmosphere. One idea is to place a planet-sized reflector between Venus and the Sun to regulate the amount of heat it receives. This would allow the carbon dioxide in the atmosphere to freeze and fall to the surface, leaving just the nitrogen in the atmosphere. 

Venus has some characteristics that make it favourable for terraforming.

• It is the closest planet to Earth. Therefore the least amount of energy will be required in transporting resources to Venus, compared to other planets.
• It has roughly the same size as the Earth and is located in the “Habitable Zone” of the sun.

However, the inhospitable conditions at its surface will have to be dealt with in order for humans to inhabit it.

• The atmosphere is extremely thick and consists of 96.5% carbon dioxide. The atmospheric pressure at the surface is a bone-crushing 90 atmospheres, and would be found on Earth at a depth of 1000 metres in the oceans.
• Carbon dioxide is a greenhouse gas and traps heat at the surface, preventing it from escaping into space. This greenhouse effect over millions of years has raised the surface temperature of Venus to a sizzling 467 degrees Celsius.
• The surface is highly volcanic, and contains over 150 volcanoes over 100 km in diameter. There are evidences of large scale lava flows on the planet

The planet Venus is often referred to as Earth’s “Sister Planet”, and rightly so. In addition to being almost the same size, Venus and Earth are similar in mass and have very similar compositions (both being terrestrial planets). As a neighboring planet to Earth, Venus also orbits the Sun within its “Goldilocks Zone” (aka. habitable zone). But of course, there are many key difference between the planets that make Venus uninhabitable.

Over the past century, the concept of terraforming Venus has appeared multiple times, both in terms of science fiction and as the subject of scholarly study. Whereas treatments of the subject were largely fantastical in the early 20th century, a transition occurred with the beginning of the Space Age. As our knowledge of Venus improved, so too did the proposals for altering the landscape to be more suitable for human habitation

By the 1950s and 60s, owing to the beginning of the Space Age, terraforming began to appear in many works of science fiction. Poul Anderson also wrote extensively about terraforming in the 1950s. In his 1954 novel, The Big Rain, Venus is altered through planetary engineering techniques over a very long period of time. The book was so influential that the term term “Big Rain” has since come to be synonymous with the terraforming of Venus

Proposed Methods:

The first proposed method of terraforming Venus was made in 1961 by Carl Sagan. In a paper titled “The Planet Venus“, he argued for the use of genetically engineered bacteria to transform the carbon in the atmosphere into organic molecules. However, this was rendered impractical due to the subsequent discovery of sulfuric acid in Venus’ clouds and the effects of solar wind

Another idea is to bombard Venus with refined magnesium and calcium, which would sequester carbon in the form of calcium and magnesium carbonates. In their 1996 paper, “The stability of climate on Venus“, Mark Bullock and David H. Grinspoon of the University of Colorado at Boulder indicated that Venus’ own deposits of calcium and magnesium oxides could be used for this process. Through mining, these minerals could be exposed to the surface, thus acting as carbon sinks

The concept of solar shades has also been explored, which would involve using either a series of small spacecraft or a single large lens to divert sunlight from a planet’s surface, thus reducing global temperatures. For Venus, which absorbs twice as much sunlight as Earth, solar radiation is believed to have played a major role in the runaway greenhouse effect that has made it what it is today

The terraforming of Venus or the terraformation of Venus is the hypotheticalprocess of engineering the global environmentof the planet Venus in order to make it suitable for human habitation. Adjustments to the existing environment of Venus to support human life would require at least three major changes to the planet’s atmosphere

1. Reducing Venus’s surface temperature of 737 K (464 °C; 867 °F)
2. Eliminating most of the planet’s dense 9.2 MPa (91 atm) carbon dioxide and sulfur dioxide atmosphere via removal or conversion to some other form
3. The addition of breathable oxygen to the atmosphere.

Eliminating the dense carbon dioxide atmosphere

The main problem with Venus today, from a terraformation standpoint, is the very thick carbon dioxide atmosphere. The ground level pressure of Venus is 9.2 MPa (91 atm; 1,330 psi). This also, through the greenhouse effect, causes the temperature on the surface to be several hundred degrees too hot for any significant organisms. Therefore, all approaches to the terraforming of Venus include somehow removing almost all the carbon dioxide in the atmosphere.

Biological approaches

The method proposed in 1961 by Carl Sagan involves the use of genetically engineeredalgae to fix carbon into organic compounds. Although this method is still proposed in discussions of Venus terraforming, later discoveries showed that biological means alone would not be successful.

Difficulties include the fact that the production of organic molecules from carbon dioxide requires hydrogen, which is very rare on Venus. Because Venus lacks a protective magnetosphere, the upper atmosphere is exposed to direct erosion by the solar wind and has lost most of its original hydrogen to space. And, as Sagan noted, any carbon that was bound up in organic molecules would quickly be converted to carbon dioxide again by the hot surface environment. Venus would not begin to cool down until after most of the carbon dioxide had already been removed

Direct removal of atmosphere

The thinning of the Venusian atmosphere could be attempted by a variety of methods, possibly in combination. Directly lifting atmospheric gas from Venus into space would probably prove difficult. Venus has sufficiently high escape velocity to make blasting it away with asteroid impacts impractical. Pollack and Sagancalculated in 1994 that an impactor of 700 km diameter striking Venus at greater than 20 km/s, would eject all the atmosphere above the horizon as seen from the point of impact, but because this is less than a thousandth of the total atmosphere and there would be diminishing returns as the atmosphere’s density decreases, a very great number of such giant impactors would be required. Landis calculated^[3] that to lower the pressure from 92 bar to 1 bar would require a minimum of 2,000 impacts, even if the efficiency of atmosphere removal was perfect. Smaller objects would not work, either, because more would be required. The violence of the bombardment could well result in significant outgassing that would replace removed atmosphere. Most of the ejected atmosphere would go into solar orbit near Venus, and, without further intervention, could be captured by the Venerian gravitational field and become part of the atmosphere once again.

Cooling planet by solar shades

Venus receives about twice the sunlight that Earth does, which is thought to have contributed to its runaway greenhouse effect. One means of terraforming Venus could involve reducing the insolation at Venus’s surface to prevent the planet from heating up again

Space-based

Solar shades could be used to reduce the total insolation received by Venus, cooling the planet somewhat. A shade placed in the Sun–Venus L₁ Lagrangian point also would serve to block the solar wind, removing the radiation exposure problem on Venus.

A suitably large solar shade would be four times the diameter of Venus itself if at the L₁point. This would necessitate construction in space. There would also be the difficulty of balancing a thin-film shade perpendicular to the Sun’s rays at the Sun–Venus Lagrange point with the incoming radiation pressure, which would tend to turn the shade into a huge solar sail. If the shade were simply left at the L₁point, the pressure would add force to the sunward side and the shade would accelerate and drift out of orbit. The shade could instead be positioned nearer to the Sun, using the solar pressure to balance the gravitational forces, in practice becoming a statite.

According to a 1991 study by British scientist Paul Birch, one way to terraform Venus is to bombard its atmosphere with hydrogen. The reaction would produce graphite and water, which would fall to the surface and cover about 80% of the planet in oceans. 

Here are some other requirements for terraforming Venus:

• Cool the planet to about 290 K 
• Reduce the atmospheric pressure to about 1 bar 
• Remove excess carbon dioxide and other poisonous atmospheric constituents 
• Provide about 0.24 bar of breathable oxygen 
• Reduce the length of the day to about 24 hours Another way to terraform Venus is to place a planet-sized reflector between Venus and the Sun. This would regulate the amount of heat the planet receives, allowing the carbon dioxide in the atmosphere to freeze and fall to the surface. Venus receives about twice the sunlight that Earth does, which is thought to have contributed to its runaway greenhouse effect. One way to terraform Venus could involve reducing the insolation at Venus’s surface to prevent the planet from heating up again. Depending on whom you talk to, terraforming could take anywhere from 50 years to 100 million years to complete. 

According to some, Venus is a more realistic option for terraforming than Mars. Here are some reasons why: 

• Gravity: Venus’s gravity is similar to Earth’s, while Mars’s gravity is only 38% of Earth’s. 
• Size: Venus is almost the same size as Earth, so it wouldn’t be as difficult for people and other life forms to adapt. 
• Atmosphere: Venus has an atmosphere, but it’s overrun with greenhouse gases. Mars has a very thin atmosphere, about 0.6% that of Earth, which can’t retain heat. 
• Air: Mars’s air is toxic and too thin to breathe. 
• Radiation: Mars also has radiation issues. However, some say that Venus is a much harder bet than Mars. Some say that Mars could be terraformed in a few thousand years, but that no gentle approach could ever work on Venus

Venus is 9 earth atmospheres at it surface. That means we would need to strip away 8 earth atmospheres from the planet just to get the pressure to where we could stand on the surface in a suit. Mars is 0.095 of Earth’s atmospheres, meaning we only need to increase pressure

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