The pressure on Venus is 1334 PSI or 92 times the pressure at sea level on Earth, which is 14.5 PSI. Now, in our oceans the pressure increases by 14.5 PSI every 33 feet. So, we're told that the atmospheric pressure on Venus is equal to the pressure on Earth at 3036 feet under the ocean? Do I have this right? If so what is causing that much pressure in a gas?

  • 4
    $\begingroup$ The pressure is caused by the gravity of Venus and the amount of gas around venus. Gravity of Venus is 90 % of Earth. The mass of the whole atmosphere of Venus is about 93 times the mass of the Earth atmosphere, see en.wikipedia.org/wiki/Venus#Atmosphere_and_climate $\endgroup$
    – Uwe
    Aug 31, 2017 at 21:20
  • $\begingroup$ Yeah, but I'm going to find out where all that gas comes from. Maybe it's the nearness to the sun. $\endgroup$ Aug 31, 2017 at 21:34
  • 2
    $\begingroup$ Given that the atmosphere on Venus is 95% CO2, the CO2 most likely originates from the volcanic activity on Venus, the same way the Earth's early atmosphere was mostly CO2 because of early volcanic activity. If it wasn't for ancient microbes using the carbon in CO2 & releasing the oxygen back into the atmosphere, Earth's atmosphere would still largely be composed of CO2. $\endgroup$
    – Fred
    Sep 1, 2017 at 12:41
  • 3
    $\begingroup$ Sorry, but most of Earth's original CO2 was converted to various calcites (CaCo3, mostly limestone) long before photosynthesis started. Water mixed with CO2 to form carbonic acid, which reacted with calcium minerals to form calcites. $\endgroup$
    – BillDOe
    Sep 1, 2017 at 20:09
  • 1
    $\begingroup$ @RichardWales Please clarify the title and text of your queston to properly reflect that you are indeed interested in how venus acquired such a heavy/dense atmosphere. Currently, your question (What causes so much pressure) and what you ask in your comment are two different things. $\endgroup$
    – Polygnome
    Sep 2, 2017 at 11:15

5 Answers 5


The pressure exerted on a surface area under the ideal gas law is $P = \frac{\rho k_B T}{\mu}$ with the following notation:

  • $\rho$ being the volume mass density (or simply density)
  • $k_B$ is the Boltzmann constant
  • $T$ is the temperature in Kelvin
  • $\mu$ is the mean molecular mass in g/mol

On Earth $\mu_E \approx 29$, while on Venus it is $\mu_V \approx 44$. Furthermore $T_E \approx 300$ and $T_V \approx 750$, so the factor of $\frac{T}{\mu}$ accounts for only a factor of $1.76$ between those pressures.
The main difference here comes from the density: $\rho_E = 1.2 kg/m^3$ while $\rho_V=67 kg/m^3$.
Together you get $P_V = P_E \cdot 1.76 \cdot 55.8 \approx 98 \cdot P_E$. The difference from this calculation compared with the factor of $92$ that is actually true, come from the fact that Venus atmosphere on the surface mostly is in a state of supercriticality, which means it is somewhere between the state of gas and fluid. This makes it necessary to apply corrections to the ideal gas law which I've not used above, for simplicity.

So the main difference in pressure comes from the higher density of Venus atmosphere. What does that mean?
There is simply so much more 'stuff' in Venus' atmosphere. Earth's total atmosphere has a mass of around $5 \cdot 10^{18}$kg, while the Venusian one has $5 \cdot 10^{20}$kg, so this is 100 times more than what Earth has.

How could this happen? Or you could ask "How can a planet nearly the same mass as Earth have an atmosphere 100 times more massive?". This is one of the big mysteries of Planet formation & evolution. There are two halfway compelling scenarios that come to my head now, both involve Earth and Venus having similar atmospheres at a relatively young age of $\sim 100$ Million years.

  1. Venus might have gotten less accretional heat in the phase as the solar system formed. Together with it's smaller size, it was able to radiate this heat away even faster than Earth was. Also smaller size implies less radiogenic heat production throughout the ages.
    All those factors might have conspired to make plate tectonics much weaker/nonexistent on Venus. This prevents burying of the atmosphere, as it happens in Earth's mantle. But it is hard / impossible to estimate how strong this effect was in the past.
  2. Venus went early into a stage of runaway greenhouse effect. We know this, because we find it today in this state. Somehow this protected the atmosphere from escaping (I don't want to specify any mechanism, as there are many possibilities), while Earth lost a significant portion of its atmosphere over time.

If you're more interested in this topic I recommend as introductory read Imke de Pater and Jack Lissauer's book "Planetary Science".

  • 1
    $\begingroup$ +1 This is a very helpful answer as it addresses what I think the OP is actually asking about, and what I think many people would like to know; How could this happen? $\endgroup$
    – uhoh
    Sep 2, 2017 at 3:12
  • $\begingroup$ In a constant volume, increasing temperature increases pressure. But the atmosphere of a planet is not a constant volume. If the temperature rises, the atmosphere gets higher, but the mass of the atmosphere over a given area does not change and pressure does not change. There are areas of lower and higher pressure on earth, but this is caused by temperature differences. But we assume here a constant temperature at the surface of the planet. $\endgroup$
    – Uwe
    Sep 3, 2017 at 23:07
  • $\begingroup$ @Uwe: What are you trying to say? Argue math and physics, not semantics. Also weather on Earth is not the same as the average state of the atmosphere on Venus. $\endgroup$ Sep 3, 2017 at 23:32
  • 1
    $\begingroup$ @Uwe: You're right in saying that this is the ideal gas law for a constant volume. But you have to check which volume you're talking about. The way the gas law is derived it is locally valid for all individual test volumes on which the density $\rho$ is defined, thus it is valid everywhere in the atmosphere. Only when phase-changes become involved it's not fully correct anymore, but I've pointed that out in my answer. $\endgroup$ Sep 4, 2017 at 11:38
  • 1
    $\begingroup$ @MagicOctopusUrn I would absolutely recommend this review article adsabs.harvard.edu/abs/2018A%26ARv..26....2L by H. Lammer et al. from last year (2018) that summarizes all the most recent understanding in a detailed manner. The article also goes into issues of solar activity with time, atmospheric escape, first accreted atmospheres, outgassed secondary atmospheres, etc. $\endgroup$ Oct 20, 2019 at 18:10

The question you did ask:
Why is the atmospheric pressure on Venus so high?

The answer is that the mass of the atmosphere of Venus is very high compared to that of the Earth, by almost a factor of 100. On the other hand, the two planets have similar surface areas and similar gravitational accelerations at the surface. Since surface pressure is approximately the weight (mass times gravitational acceleration) of the atmosphere divided by the surface area, this means that surface pressure on Venus is very high compared to that of the Earth, by almost a factor of 100.

This leads to the question you didn't ask:
Why is the atmosphere of Venus so massive (and why is it almost all CO2)?

The answer to this question is that the Earth has water on the surface, plate tectonics, and abundant life. Venus has none of these.

The combination of the above means that Earth has a vigorous carbonate-silicate cycle that sequesters vast amounts of carbon underground. This cycle does not exist on Venus. Venus has instead expelled a large amount of its crustal carbon into its atmosphere, mostly in the form of carbon dioxide.

  • 1
    $\begingroup$ Interesting answer. Does the argument apply to Mars as well? Mars does not have a crushing CO2 atmosphere because it (once) had a carbonate-silicate cycle? Let's give this hypothesis a test drive. $\endgroup$
    – uhoh
    Sep 2, 2017 at 11:56
  • $\begingroup$ Carbonate cycle is all well and good, but is this mechanism able to bury 91 atmospheres of material? Would also be interested in references for this. $\endgroup$ Sep 2, 2017 at 15:50
  • $\begingroup$ @uhoh - Mars is too small to hold onto a substantial atmosphere. $\endgroup$ Sep 2, 2017 at 16:04
  • 1
    $\begingroup$ It's pretty amazing that Venus can have 100 x Earth atmosphere but Mars only 0.01 x Earth atmosphere just because of the size difference. Also I thought Mars' problem was the lack of magnetic field? $\endgroup$
    – uhoh
    Sep 2, 2017 at 16:11
  • $\begingroup$ On Earth there is not only the carbonate-silicate cycle, there is also the en.wikipedia.org/wiki/Carbon_cycle, both are removing carbon dioxide from the atmosphere. But both cycles are not possible on Venus due to the high temperature and the lack of photosynthesis. On Earth, a lot of oxygen removed by photosynthesis from carbon dioxide was bound in metall oxides long ago, for instance iron ore. $\endgroup$
    – Uwe
    Sep 3, 2017 at 14:25

Atmospheric pressure (or water pressure, for that matter) is simply the weight of the atmosphere that one square inch (or any square unit) supports. The atmospheric pressure on earth is, for the sake of argument, 14.5 PSI. That simply means that there is 14.5 pounds of atmosphere above one square inch of surface at sea level on Earth. (To calculate the pressure at a given depth in the ocean, you only need to calculate the weight of the ocean above that depth.) As @Uwe pointed out in comments, the mass of the atmosphere on Venus is 93 times that of Earth's, so one would expect that the surface pressure would be that much greater, as well.


The atmosphere of Venus up to 48 km comprises high velocity jetting of sulfur (SN) gas through over 1,000,000 ‘small domes’ imaged by Soviet and NASA Magellan radar. SN gas, the normal form of sulfur at the temperature in the lower atmosphere, jets at high speed until it reaches the altitude (temperature) at which it crystallizes to form a monoclinic crystal and due to the heat released rises a few km to the temperature level where it changes to a rhombic crystal. The denser rhombic crystals fall downward and revert to the monoclinic form which, the change of which is completely reversible. This produces the the thin roiling lower cloud layer, the mass of which, along with the jetting SN and CS produce the high pressure at the surface.

The Lower Cloud Layer (LCL)forms the boundary between the two modes of Venus’ bi-modal atmosphere, where different molecular species and pressure altitude relationships attain. Changes in molecular species with elevation can only occur in such a ‘mass flow’ environment. The original Pioneer Venus figure showed the physical layers and temperatures of each as a function of altitude, but the chemical composition above and below the LCL were not be determined.

A three order-of-magnitude drop in the Pioneer Venus CO2 mass spec channel at the LCL altitude was interpreted as a clogging of the inlet leaks (there were two at the time). The mass 44 counts remained low until PV descended to 31 km, the bottom of the red-haze layer, where the channel 44 counts recovered. This was attributed to the evaporation of the occluding droplets and the counts below 31-km were assumed to be CO2. The crystallization temperatures of monoclinic and orthorhombic S8 correspond exactly with the temperature at the LCL. The mass spectrometer not detect the S8 because the mass of the S8 molecule, 256.47 amu is beyond the range of the mass spectrometer instrument, 208 amu.

Carbon Sulfide, CS, occupies the entire lower atmosphere of Venus along with S8. What scientists expected to be CO2 below 31 km is actually CS (carbon sulfide), ‘masquerading’ as CO2. CS and CO2 have very similar masses – 44.0686 and 44.0096 amu, respectively. The evidence indicating CS in the lower atmosphere is present in the form of the red haze observed from 31 km up to the LCL. Again, a simple look-up of the temperature at which rising hot CS gas would form small red crystals (200 C) coincides exactly with the lower level of the red haze.

ref: http://firmament-chaos.com/papers/Venus-Paper-2018.pdf

  • 1
    $\begingroup$ Welcome to Space! This is a really interesting answer to read. I'd like to make a few recommendations for how to make this a better Stack Exchange answer. 1) please include some supporting links, references or citations. Without those, there is no way for future readers to judge how accurate this information is. 2) Make sure that you clearly mark which part of the answer directly addresses the question as asked: "Why is the atmospheric pressure on Venus so high?" and " ...what is causing that much pressure in a gas?" Thanks! $\endgroup$
    – uhoh
    Oct 20, 2019 at 3:50
  • $\begingroup$ Thanks for the link! $\endgroup$
    – uhoh
    Oct 22, 2019 at 0:10

Yes you are right. There is a lot more and heavier gas on Venus than on Earth, and since Venus is smaller than Earth, the pressure that the gas exerts per square inch is much higher.

Here is a good comparison between the two planets. Notice that according to Dr Soper's table, there are 66 molecules per square meter on Venus, versus only 1 on Earth.

  • 1
    $\begingroup$ "since Venus is smaller than Earth, the pressure that the gas exerts per square inch is much higher" What does that mean? $\endgroup$ Sep 1, 2017 at 16:57
  • 1
    $\begingroup$ There are much more molecules per square meter than only 66. Carefully read the explanation of Dr. Soper's table. $\endgroup$
    – Uwe
    Sep 1, 2017 at 21:04

Your Answer

By clicking “Post Your Answer”, you agree to our terms of service, privacy policy and cookie policy

Not the answer you're looking for? Browse other questions tagged or ask your own question.