NuclearVacuum's work

NuclearVacuum wrote: Here is some of my planetary work

Sirius_Alpha wrote:For your Gliese 581 c image, are you able to get Mie rendering on your computer with Celestia? That might make the atmosphere look much more realistic, as opposed to being an outline of the planet.

If I remember correctly, pressing Ctrl + v will cycle through rendering options.

NuclearVacuum wrote:Hm... I have never heard of anything like that. So I would say, it doesn't have that anymore.

Edasich wrote:I suppose. I'm not so fond of physics at all

A back-of-the-excel calculation using the Gonzalez and Laws (2008) numbers tells me that the HD28185 system should be dryer than bone. The solar composition has enough O such that you can have all the metals oxidized, all the carbon oxidized to CO, and still have O left over to combine with H to form water. Using the numbers from the arxiv version of the above paper, the high metals, high carbon, but solar oxygen means that with all the metals less electronegative than H oxidized, you don’t have enough O left over to oxidize all the C to CO. So instead of a solar-type nebula buffered by H2-CO-H2O, you are in H2-CO-CH4 space. No water, no steam, no ice. And condensation above the CH4 decomposition temperature might even give you a hybrid silicate-carbon planet. caveat: this is simple late-night stochiometric calc, not a proper thermodynamic fractionation run. caveat 2: I normalized their values to Asplund et al. 2004’s solar values. Since Asplund paper isn’t referenced by Gonzalez and laws, they may be normalizing their stellar metal values to a different solar composition, in which case my numbers will be wrong.

Sirius_Alpha wrote:About HD 28185's moon, someone on the Oklo blog wrote.

A back-of-the-excel calculation using the Gonzalez and Laws (2008) numbers tells me that the HD28185 system should be dryer than bone. The solar composition has enough O such that you can have all the metals oxidized, all the carbon oxidized to CO, and still have O left over to combine with H to form water. Using the numbers from the arxiv version of the above paper, the high metals, high carbon, but solar oxygen means that with all the metals less electronegative than H oxidized, you don’t have enough O left over to oxidize all the C to CO. So instead of a solar-type nebula buffered by H2-CO-H2O, you are in H2-CO-CH4 space. No water, no steam, no ice. And condensation above the CH4 decomposition temperature might even give you a hybrid silicate-carbon planet. caveat: this is simple late-night stochiometric calc, not a proper thermodynamic fractionation run. caveat 2: I normalized their values to Asplund et al. 2004’s solar values. Since Asplund paper isn’t referenced by Gonzalez and laws, they may be normalizing their stellar metal values to a different solar composition, in which case my numbers will be wrong.