![]() I was pointing out a possible reason for why your black earth was not the same, hence why I mentioned the climate. No, I wasn't implying it would make it inaccurate, I just said the climate model in US2 changes a saved planet's look, like water and ice, when placed in a new simulation. In that light, locking parameters enables you to simulate something you don't know the cause of but want to see the effect. A magnetic field of 2.5+ radii should make sure your planet doesn't get "stripped"Īnyway, although the argument, changing the starting parameters of a simulation wouldn't be scientifically correct is pretty invalid 1), there is nothing to say against optional parameter locks.ġ)Being able to change the starting parameters of a simulation is the only thing that makes a simulation scientifically useful. At the right temperature the surface water will compensate the atmosphere loss for a time, lowering the surface water level but it keeps escaping. However, if you place the planet in a running sim, it has no magnetic field at all and the atmosphere will escape. Putting a saved planet will set its effective temperature correctly but the surface takes a bit to actually reach the right temperature (which at Albedo 0.3 is roughly effective temperature+ greenhouse effect=surface temperature). We will probably change this at some point to more realistically cover the in-between states and expose what's going on.The changes after placing a saved planet in a new sim occur due to the magnetic field and the surface temperature not being saved. So any time you add a random rocky planet, when it crosses an arbitrary atmosphere mass threshold it will stop paying attention to the Infrared Emissivity value, and start behaving more like Venus. So we use an equation for an optically-thick dry troposphere runaway greenhouse limit, which depends on other parameters and is calibrated for Venus. You would need an infrared emissivity much greater than 1, which doesn't really make sense. The trouble is that this conceptualization does not work for very thick atmospheres like Venus. Usually for rocky planets we use a single layer atmosphere with an infrared emissivity, as referred to in the third item of the FAQ. In answer to the question, you have indeed observed a discontinuity in the way we calculate temperature for very thick atmospheres. It clearly implements some aspects like the Stefan–Boltzmann law and non-ideal body properties for absorbance and emission, but some of the numerical results like those dramatic shifts don't make much sense to me. I guess my question boils down to what the mathematical model of the surface temperature is right now. I have doubts that such a dramatic shift around that transition really fits well with reality and expectations of game mechanics. The more predictable rise with significantly more mass makes sense, but that already sits well with me. Depending on the parameters for albedo and IR emissivity, I've seen shifts in the greenhouse effect as large as starting at +50 K and crash to near 0 K when crossing over that point (~1% increase) in atmospheric mass. In particular, the changes in atmospheric mass around that critical ratio can cause dramatic shifts in the temperature rise due to the greenhouse effect (or at least what is called such in the program). My question relates to reconciling what I see in the game with reality. What you said makes sense in regards to reality and physical models. Also while (visible) light is escaping the planet it's wavelength slightly shifts towards red and eventually infrared, contributing to the effect because visible light is also reflected and hence bounces as well, shifting a little towards red each time it goes "up". With a thick layer of atmosphere containing reflective stuff the IR light of both sources will hit the surface more often, bouncing between surface and greenhouse contributors. ![]() Infrared Emissivity mostly refers to your planet cooling down and not so much to reflecting light of IR wavelength. Below that ratio, gases would simply escape. Pressure and gravity are working against each other and it's only at and above a certain M atmosphere / M planet ratio that gravity gets the upper hand. For the same reason the pressure will go up with more atmosphere mass. The more massive a planet is the more atmosphere it takes to get the atmosphere reach higher above the surface, because of gravity. Scale Height is playing a big role once the atmosphere passes a certain mass relative to the planet's mass.
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