Inputs

Each of the inputs are listed below. The order of each input type does not matter. EOM searches for the specific headers (including the # sign) and reads the information accordingly. The order of the parameters within each type does need to be as written here. An example input file is created upon installation. The user should examine this file and modify as necessary prior to running the code.

Required: #OUTPUT:

#OUTPUT
dtOut         (float)
nOutputTypes  (int)
outputtype1   (str)
outputtype2   (str)
...

Specify output. dtOutput is the number of seconds between writing output. nOutputTypes specifies the number of output types to write. Then, each outputtype must be specified. See output.py for complete list.

Current output types are ALL, PHOTO, and USER. ALL and PHOTO are filled with specific values of interest.

USER is meant to be more flexible. The user can add a set of values to an array without needing to write a bunch of code in output.py. See user.py for instructions.

Required: #TSTART:

#TSTART
year
month
day
hour
minute
second

The end time of the simulation

Required: #TEND:

#TEND
year
month
day
hour
minute
second

The end time of the simulation

Required: #TSTEP:

#TSTEP
nseconds

The time step. The time step depends on the irradiance specified in the model and the chemical scheme used. Testing should be done when changing these things to determine the appropriate time step.

Required: #USEPHOTODATA:

#USEPHOTODATA
T or F
irradiancefile

If T, observations of the solar irradiance at the top of the atmosphere are used. EOM then reads the irradiance from the file specified

If F, EOM assumes blackbody and calculates the irradiance based on the parameters set using the #RADIATIONPARAMETERS flag and the irradiance file is ignored.

Required: #ATMOSPHERE:

#ATMOSPHERE
Pressure/Pressure_Earth
O2MixingRatio

Specifies fundamental values used for setting up the background atmosphere.

Required: #STAR:

#STAR
Tstar
Rstar/Rsun

Stellar parameters for radiation calculation purposes.

Required: #PLANET:

#PLANET
planetDistanceAU
rPlanet/rEarth
mPlanet/mEarth
eccentricity
nDaysInYear
solarZenithAngle

Fundamental parameters to set up the radiation environment and determine orbital distance. Note: if the irradiance is specified at the top of the atmosphere (e.g. by data), an eccentricity of 1 should be used.

Required: #CHEMISTRY:

#CHEMISTRY
simple or backwardEuler

Simple chemical solver assumes photochemical equilibrium for certain species. backwardEuler makes no such assumption and the Backward Euler implicit scheme is used.

Optional: #TEMPERATURE:

#TEMPERATURE
scaled/isothermal/equilibrium/
parameter1
parameter2
...

There are a few different ways to calculate/specify the temperature. If this option is not used, then the temperature is read from a file located in input/ustspline.txt and held constant. This file is required regardless of the temperature method specified as it sets up the vertical coordinate and the initial pressure.

Scaled: the temperature is initialized using the values in input/ustspline.txt and then scaled depending on the orbital position. Required parameters: 1 ScaleFactor float; Multiply initial temperature by this factor at perihelion

isothermal: Use isothermal temperature profile Required parameters: 1 Temperature float; the temperature of the atmosphere

equilibrium: calculate the equilibrium temperature based on stellar and planetary parameters (stellar parameters are specified using #STAR flag, see above). Required parameters: 2 albedo float; surface albedo emmissivity float; emmissivity (0.67 for Earth)

Optional: #STEADYSTATE:

#STEADYSTATE
T/F               (logical)
stoppingCriteria  (float)

If true, run the model until a steady state has been reached, defined by the stopping criteria (as a percent difference). Setting this to T means that any #TEND condition that is specified will be ignored. If this option is not specified, or is specified as F, then #TEND is used as the stopping condition.