<p>The early atmospheres of Venus, Earth and Mars all had a lot of CO2, Carbon and oxygen are some of the most common elements in molecular clouds, and so it is no surprise that their most common and stable compound should be common in atmospheres.  </p>

<p>On the Earth, life happened.</p>

<p>The carbon in the atmosphere was fixed by autotrophs (particularly blue-green algae and the later plants) into the bodies of living things, and then into rocks formed from those bodies: Chalk, Limestone, Coal and Oil. This left an atmosphere dominated by Nitrogen, and later by the toxic waste products from those algae: oxygen.</p>

<p>Mars was too small to hold onto lighter gases like Nitrogen, and these escaped into space, there is just a trace of the heavier gases: CO2, but at a very low pressure.</p>

<p>Venus retains a dense atmosphere dominated by CO2</p>

CC BY-SA 3.0
2017-09-27T18:16:53.410Z
2017-09-27T18:16:53.410Z
James K
<p>In addition to James K's answer, many gases exist in the disk of material that forms into planets.   What's a gas as opposed to a liquid or solid also depends on temperature and pressure.   The most abundant "gases" in our solar-system are hydrogen, helium, CO2, H2O, CH4, NH3, N2, O2, CO, Neon (and maybe some others I've overlooked), in something sort of close to that order.   Many of these "gases" are also ices that form up the majority of comets.</p>

<p>During planetary formation, the ring of debris is too warm for hydrogen,  Helium and Neon to be anything but a gas, though some hydrogen is bound to heavier elements and abundant in planet formation.  Helium and Neon and the other Noble Gases don't bind well with other elements. </p>

<p>The other abundant "gases", H20, CO2, NH3, CH4, etc, can exist as ices past their respective <a href="https://en.wikipedia.org/wiki/Frost_line_(astrophysics)" rel="nofollow noreferrer">frost lines</a>.   That's why those molecular compounds are much more common in the outer part of the solar system.   </p>

<p>Earth and Mars formed inside the frost-line so they formed mostly out of rocky material, after which, much of the lighter elements, primarily gases and liquids, were acquired by comet impacts after formation, though some probably existed prior too formation.   </p>

<p>During the late heavy bombardment there were many large impacts and one consequence of very large comet or meteor impacts is a rise in temperature, so, even in the early solar-system when the sun wasn't as luminous as it is now, the planets, Earth and Mars spent some of the time quite hot.</p>

<p>There's two primary ways a planet can lose it's atmosphere, <a href="https://en.wikipedia.org/wiki/Atmospheric_escape" rel="nofollow noreferrer">Jeans Escape</a> and by the solar wind.  </p>

<p>The solar wind is made up of almost entirely charged particles, so if a planet has a magnetic field, the impact of those high speed particles is largely deflected, where as, if they impact the upper atmosphere, the planet can lose it's atmosphere like tiny billiard balls being knocked off one at a time.</p>

<p>While the method of those two ways a planet can lose it's atmosphere are different, it comes down to basically the same thing.   When gas molecules on the outer edge of a planet's atmosphere move faster than escape velocity they are likely to escape the planet into space and because lighter gas molecules move faster than heavier ones.   That's the <a href="https://en.wikipedia.org/wiki/Maxwell%E2%80%93Boltzmann_distribution" rel="nofollow noreferrer">Maxwell-Boltzmann law</a> or <a href="https://en.wikipedia.org/wiki/Root-mean-square_speed" rel="nofollow noreferrer">Root-mean-square formula</a>, planets are more likely to retain heavier gases.</p>

<p>Venus and Mars have both lose most of their lighter gases, H20, CH4, NH3 but CO2 is heavy enough to have been retained by both those planets, though it's worth pointing out that we don't know how much CO2 Mars had millions and billions of years ago.   Mars may have lost much of it's CO2 over time as well.  It just lost it more slowly than the lighter gases.   Mars was able to retain some of it's water, however, in the form of ice.</p>

<p>Venus, like Mars, lost nearly all of it's gaseous water.   We know that Venus used to have much more water because it's very high <a href="http://www.nature.com/nature/journal/v363/n6428/abs/363428a0.html?foxtrotcallback=true" rel="nofollow noreferrer">D to H ratio</a> wouldn't be possible unless it had lost a significant percentage of it's water, likely 99.9% or higher. </p>

<p>Earth is massive enough and Earth has a strong magnetic field, so Earth is able to retain it's lighter gases like CH4, NH3 and atmospheric H20, though Earth loses Hydrogen and Helium to space.    NH3 is kind of interesting because it dissolves in water quite readily, so as soon as the young Earth had oceans, those oceans were likely Ammonia/water with whatever else readily dissolved in the liquid such as Iron.   The early oceans are thought to have been brown colored from the dissolved Iron.  But Earth's young atmosphere was likely mostly CO2 and CH4 with most of the H20 in liquid form, (and at times, much of it was ice).</p>

<p>As life and photosynthesis began releasing Oxygen, Oxygen readily bonded with the CH4 and dissolved Iron in the oceans, turning the oceans blue and in time, making the Atmosphere free of CH4 and more abundant with O2.   It's unclear (and perhaps unlikely?) if Mars and Venus ever underwent that Oxygenation period that Earth did.   Having abundant liquid oceans and having photosynthetic life made a significant difference to Earth's atmosphere.   </p>

<p>You mentioned plate tectonics and that plays a role too as does the chemistry that happens in the oceans and below the surface of a planet.    The main reason Mars is 95% CO2 now is because it's small and it doesn't have a good magnetic field, only small localized ones.    It lost most of it's atmosphere and nearly all of it's lighter gas molecules.</p>

CC BY-SA 3.0
2017-09-27T19:18:11.380Z
2017-09-27T19:18:11.380Z
userLTK
<p>As far as I know, Earth and Mars were relatively similar when the solar system formed. So most of the CO2 was used to form carbonic rocks (right?). I found that tectonic movements are the reason that the CO2 on Earth could be released again, which don't exist on Mars. </p>

<p>So how comes that the atmosphere has 95% CO2?</p>

CC BY-SA 3.0
2017-09-27T16:40:51.400Z
Are you asking why it has such a high fraction of CO2 (as opposed to the relatively small fraction here on Earth) or why it has the quantity of CO2 it has? Because those will be different answers.
zephyr
CC BY-SA 3.0
2017-09-27T19:48:50.713Z
Firstly, you have to realize that Mars has 1/100th of the atmospheric pressure of Earth. That means the atmosphere is roughly a factor 100 less massive, means 100 times fewer molecules than on Earth. Add burying carbon by geology and biomass, and $O_2$ release into the atmosphere, and it's not that much of a difference.
AtmosphericPrisonEscape
<planetary-atmosphere><mars>
Where does the CO2 in Mars atmosphere come from?
Amiris
# Where does the CO2 in Mars atmosphere come from?

(Asked by: username_0 on 2017-09-27)

As far as I know, Earth and Mars were relatively similar when the solar system formed. So most of the CO2 was used to form carbonic rocks (right?). I found that tectonic movements are the reason that the CO2 on Earth could be released again, which don't exist on Mars.

So how comes that the atmosphere has 95% CO2?

**Tags:** planetary-atmosphere, mars

> **Comments:**
> **username_1**: Are you asking why it has such a high fraction of CO2 (as opposed to the relatively small fraction here on Earth) or why it has the quantity of CO2 it has? Because those will be different answers.  
> **username_2**: Firstly, you have to realize that Mars has 1/100th of the atmospheric pressure of Earth. That means the atmosphere is roughly a factor 100 less massive, means 100 times fewer molecules than on Earth. Add burying carbon by geology and biomass, and $O_2$ release into the atmosphere, and it's not that much of a difference.  

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## 2 answers

### Answer by username_3 on 2017-09-27. Score: 6

The early atmospheres of Venus, Earth and Mars all had a lot of CO2, Carbon and oxygen are some of the most common elements in molecular clouds, and so it is no surprise that their most common and stable compound should be common in atmospheres.

On the Earth, life happened.

The carbon in the atmosphere was fixed by autotrophs (particularly blue-green algae and the later plants) into the bodies of living things, and then into rocks formed from those bodies: Chalk, Limestone, Coal and Oil. This left an atmosphere dominated by Nitrogen, and later by the toxic waste products from those algae: oxygen.

Mars was too small to hold onto lighter gases like Nitrogen, and these escaped into space, there is just a trace of the heavier gases: CO2, but at a very low pressure.

Venus retains a dense atmosphere dominated by CO2


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### Answer by username_4 on 2017-09-27. Score: 3

In addition to username_3's answer, many gases exist in the disk of material that forms into planets. What's a gas as opposed to a liquid or solid also depends on temperature and pressure. The most abundant "gases" in our solar-system are hydrogen, helium, CO2, H2O, CH4, NH3, N2, O2, CO, Neon (and maybe some others I've overlooked), in something sort of close to that order. Many of these "gases" are also ices that form up the majority of comets.

During planetary formation, the ring of debris is too warm for hydrogen, Helium and Neon to be anything but a gas, though some hydrogen is bound to heavier elements and abundant in planet formation. Helium and Neon and the other Noble Gases don't bind well with other elements.

The other abundant "gases", H20, CO2, NH3, CH4, etc, can exist as ices past their respective [frost lines](https://en.wikipedia.org/wiki/Frost_line_(astrophysics)). That's why those molecular compounds are much more common in the outer part of the solar system.

Earth and Mars formed inside the frost-line so they formed mostly out of rocky material, after which, much of the lighter elements, primarily gases and liquids, were acquired by comet impacts after formation, though some probably existed prior too formation.

During the late heavy bombardment there were many large impacts and one consequence of very large comet or meteor impacts is a rise in temperature, so, even in the early solar-system when the sun wasn't as luminous as it is now, the planets, Earth and Mars spent some of the time quite hot.

There's two primary ways a planet can lose it's atmosphere, [Jeans Escape](https://en.wikipedia.org/wiki/Atmospheric_escape) and by the solar wind.

The solar wind is made up of almost entirely charged particles, so if a planet has a magnetic field, the impact of those high speed particles is largely deflected, where as, if they impact the upper atmosphere, the planet can lose it's atmosphere like tiny billiard balls being knocked off one at a time.

While the method of those two ways a planet can lose it's atmosphere are different, it comes down to basically the same thing. When gas molecules on the outer edge of a planet's atmosphere move faster than escape velocity they are likely to escape the planet into space and because lighter gas molecules move faster than heavier ones. That's the [Maxwell-Boltzmann law](https://en.wikipedia.org/wiki/Maxwell%E2%80%93Boltzmann_distribution) or [Root-mean-square formula](https://en.wikipedia.org/wiki/Root-mean-square_speed), planets are more likely to retain heavier gases.

Venus and Mars have both lose most of their lighter gases, H20, CH4, NH3 but CO2 is heavy enough to have been retained by both those planets, though it's worth pointing out that we don't know how much CO2 Mars had millions and billions of years ago. Mars may have lost much of it's CO2 over time as well. It just lost it more slowly than the lighter gases. Mars was able to retain some of it's water, however, in the form of ice.

Venus, like Mars, lost nearly all of it's gaseous water. We know that Venus used to have much more water because it's very high [D to H ratio](http://www.nature.com/nature/journal/v363/n6428/abs/363428a0.html?foxtrotcallback=true) wouldn't be possible unless it had lost a significant percentage of it's water, likely 99.9% or higher.

Earth is massive enough and Earth has a strong magnetic field, so Earth is able to retain it's lighter gases like CH4, NH3 and atmospheric H20, though Earth loses Hydrogen and Helium to space. NH3 is kind of interesting because it dissolves in water quite readily, so as soon as the young Earth had oceans, those oceans were likely Ammonia/water with whatever else readily dissolved in the liquid such as Iron. The early oceans are thought to have been brown colored from the dissolved Iron. But Earth's young atmosphere was likely mostly CO2 and CH4 with most of the H20 in liquid form, (and at times, much of it was ice).

As life and photosynthesis began releasing Oxygen, Oxygen readily bonded with the CH4 and dissolved Iron in the oceans, turning the oceans blue and in time, making the Atmosphere free of CH4 and more abundant with O2. It's unclear (and perhaps unlikely?) if Mars and Venus ever underwent that Oxygenation period that Earth did. Having abundant liquid oceans and having photosynthetic life made a significant difference to Earth's atmosphere.

You mentioned plate tectonics and that plays a role too as does the chemistry that happens in the oceans and below the surface of a planet. The main reason Mars is 95% CO2 now is because it's small and it doesn't have a good magnetic field, only small localized ones. It lost most of it's atmosphere and nearly all of it's lighter gas molecules.


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