Update 7/31

  • Need to move out of 476 for a week or two. What should we do with computers/where should we store miscellany?
  • ​Parameter space paper essentially done. If we want input from Ruth, we should set up a time to talk with her. I'll give it a final once-over, then submit.
  • First cut of intro and methods for ​radiation pressure paper. Introduction may need to go a little deeper into a discussion of the wind itself - could use some input here. Also, I've pulled most of the methods from the parameter space paper.
  • HD209458b status: These two frames compare almost the same amount of physical time:

http://www.pas.rochester.edu/~adebrech/PlanetIonization/radPress/HD209458b_larger_r.png

http://www.pas.rochester.edu/~adebrech/PlanetIonization/radPress/HD209458b_solar_ionizing0044.png

The wind is building much more slowly. Based on Owen & Alvarez 2015, we're well into the cooling-limited regime here. This seems relatively borne out by the heating and cooling happening:

http://www.pas.rochester.edu/~adebrech/PlanetIonization/radPress/heating-cooling.png

Doing a calculation similar to that for the radiation pressure blowoff (but I believe more accurate - fewer unknown factors here), without cooling, we would expect the mass between the ambient and Rp to be completely unbound in CT ([min flux, med flux, max flux]), compared to CT for our heavier parameter space planet (which is on the high side, but not too far off - plus, we're not launching all of the mass considered here). This suggests it will take ~50x longer to launch the wind with HD209458 There's no explicit dependence on planet radius, but changing the radius also changes the density (which is why these differ, in addition to the additional planet mass). Louden et al.​ reconstructed a lower total ionizing flux (a factor of ½) than we're using, but we could increase the flux to get a stronger wind.

  • I believe charge exchange should be working now, with the stellar wind also implemented as required. I have the stellar wind set to maintain in the -x, y boundaries (y because there's the rotational component of the interaction). Waiting for the most recent test to start (requires more RAM than available on debug partition).

To Do

  • Still contemplating the ​blowoff threshold. Eric has suggested cooling as a possible mechanism; I'd also like to include some sort of ablation, since the outside layers can absorb a lot more energy than required to unbind them before they're no longer shielding the inner gas (this is partially because we assume the gas absorbs at line center, no matter its radial velocity - this may be more important than we were initially thinking).
  • Finalize charge exchange. Will test against analytic 1D solution; anything else we can test against?
  • Continue HD209458b radiation pressure.

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