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mfb said:Why do you expect a linear relationship between g on the surface and atmospheric pressure?
Without solar wind, the key quantity is the average kinetic energy of the molecules (in the upper atmosphere) compared to the energy necessary to escape from the planet. The escape velocity is about 5 km/s for Mars, for Earth it is 11.2 km/s.
Let's take Earth: T=2000 K, E=3/2 kT = 250 meV (the hot temperature is driven by solar radiation).
The necessary energy to escape for Helium is ##\frac{1}{2} m_{He} v^2_{esc} = 2.6 eV = 10.4 * 250 meV.
While it is rare, some helium atoms will get 10 times their average energy (and move upwards), and escape. Over geological timescales, most helium atoms escape.
Elementary nitrogen needs 3.5 times this energy, or ~35 times the average energy. That is really rare. Molecular nitrogen needs even more energy.
=> on Earth, helium escapes, but nitrogen does not (not including effects of solar wind).
Sorry, but still don't understand it fully. So escape speed is half on Mars (compared to Earth), kinetic energy is divided by four. But the rad dose from Sun is also about half (based on square of distance). That makes me think (of course i can be wrong), that chance to escape is twice that much, is that enough for such thin air?
Lighter elements also escape from Earth. Isnt it possible, that while lighter elements escaped from Mars, the heavier ones (nitrogen, molecules with oxygen) are rather frozen, captured by regolith?
How can we estimate the amount of ice on the caps?
About the speculation, what can be underground : https://www.nasaspaceflight.com/2015/09/nasa-confirms-salt-water-flows-mars/