I've been trying to figure out a model (or find a relevant paper) for calculating the approximate day/night and periapsis/apoapsis temperature variation for an earth-like planet that has a high eccentricity and a slow rotation rate. The planet orbits an M-class star, and is slightly smaller than earth with a thicker atmosphere of primarily nitrogen and oxygen.
Mass of the atmosphere and the size of the oceans play a key role in the retention and redistribution of heat. However I've been unable to locate any research papers or explicit models that would help me figure out specifics of how much of the temperature variation would be mitigated by retention and redistribution.
Here are the key characteristics of the planet:
- 27-day orbit
- 13.5-day (324 hour) rotation (2:1 orbital resonance)
- 27-day solar day (sunrise to sunrise)
- 0 obliquity
- 0.24 eccentricity
- 3 bar surface atmospheric pressure
- 1476 W/m^2 solar flux (based on semimajor axis)
- apoapsis: 0.16 AU
- periapsis: 0.099 AU
- semimajor axis: 0.13 AU
- 11.5C mean temperature (based on semimajor axis, flux, etc.).
Anything...even simply links to applicable research papers would be immensely helpful. Thanks!