J/A+A/574/A35 Analytical model for irradiated atmospheres (Parmentier+, 2015)
A non-grey analytical model for irradiated atmospheres.
II: Analytical vs. numerical solutions.
Parmentier V., Guillot T., Fortney J., Marley M.
<Astron. Astrophys. 574, A35 (2015)>
=2015A&A...574A..35P 2015A&A...574A..35P
ADC_Keywords: Models, atmosphere ; Planets
Keywords: radiative transfer - planets and satellites: atmospheres -
stars: atmospheres - planet-star interactions
Abstract:
This code computes the analytical pressure-temperature profile using
the non-grey analytical model of Parmentier & Guillot
(2014A&A...562A.133P 2014A&A...562A.133P, Cat. J/A+A/562/A133). Given the different
options (explained below) it can use the coefficients from Parmentier
et al. (2014A&A...562A.133P 2014A&A...562A.133P, Cat. J/A+A/562/A133) and/or the Rosseland
opacity functional form of Valencia et al. (2013) based on the
Rosseland opacities of Freedman et al. (2008ApJS..174..504F 2008ApJS..174..504F)
While using this code for publication, please cite
Parmentier & Guillot (2014A&A...562A.133P 2014A&A...562A.133P). If the options
"COEFF=AUTO" or "ROSS=AUTO" are used, please cite Parmentier et al.
(2014, this paper) and Valencia et al. (2013ApJ...775...10V 2013ApJ...775...10V)
respectively.
The code and all the outputs uses SI units.
Description:
The model has six parameters to describe the opacities:
- κ(N) is the Rosseland mean opacity at each levels of the
atmosphere it does not have to be constant with depth.
- Gp is the ratio of the thermal Plank mean opacity to the thermal
Rosseland mean opacity.
- Beta is the width ratio of the two thermal bands in the frequency
space.
- Gv1 is the ratio of the visible opacity in the first visible band
to the thermal Rosseland mean opacity
- Gv2 is the ratio of the visible opacity in the second visible band
to the thermal Rosseland mean opacity
- Gv3 is the ratio of the visible opacity in the second visible band
to the thermal Rosseland mean opacity
Each visible band has a fixed width of 1/3.
Additional parameters describe the physical setting:
- Teq0 is the equilibrium temperature of the planet for 0 albedo
and full redistribution of energy.
- mu is the angle between the vertical direction and the stellar
direction. For average profiles set mu=1/sqrt(3)
- f is a parameter equal to 0.5 to compute a dayside average profile
and 0.25 for planet average profile.
- Tint is the internal temperature, given by the internal luminosity
- grav is the gravity of the planet
- Ab is the Bond albedo of the planet
- P(i) are the pressure levels where the temperature is computed.
- N is the number of atmospheric levels.
Several options are available in order to use the coefficients derived
in Parmentier et al. (2014A&A...562A.133P 2014A&A...562A.133P, Cat. J/A+A/562/A133):
ROSS can take the values :
- "USER" for a Rosseland mean opacity set by the user
κ(nlevels) through the atmosphere.
- "AUTO" in order to use κ(P,T), the functional form of the
Rosseland mean opacities provided by Valencia et al.
(2013ApJ...775...10V 2013ApJ...775...10V) and based on the opacities calculated by
Freedman et al. (2008ApJS..174..504F 2008ApJS..174..504F).
The value of κ is then recalculated and the initial value set
by the user is NOT taken into account.
COEFF can take the values :
- "USER" for coefficients set by the user
- "AUTO" for using the fit of the coefficients provided in
Parmentier et al. (2014A&A...562A.133P 2014A&A...562A.133P, Cat. J/A+A/562/A133).
In that case all the coefficients set by the user are NOT
taken into account (apart for the Rosseland mean opacities)
COMP can take the values (Valid only if COEFF="AUTO") :
- "SOLAR" to use the fit of the coefficients for a solar
composition atmosphere
- "NOTIO" to use the fit of the coefficients without TiO
STAR can take the value (Valid only if COEFF="AUTO"):
- "SUN" to use the fit of the coefficients for a sun-like
stellar irradiation
ALBEDO can thake the value :
- "USER" for a user defined albedo
- "AUTO" to use the fit of the albedos for solar-composition,
clear-sky atmospheres
CONV can be either :
- "NO" for a pure radiative solution
- "YES" for a radiative/convective solution (without taking
into account detached convective layers)
The code and all the outputs uses SI units.
Installation and use :
to install the code use the command "make". To test use "make test".
The test should be done with the downloaded version of the code,
without any changes. To execute the code, once it has been compiled,
type ./NonGrey in the same directory.This will output a file
PTprofile.csv with the temperature structure in csv format and a file
PTprofile.dat in dat format.
The input parameters must be changed inside the file paper2.f90. It is
necessary to compile the code again each time. The subroutine
tprofile2e.f90 can be directly implemented into one's code.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
paper2.f90 204 154 Main program
tprofile.f90 512 40 Subroutine calculating the profile
valencia.f90 260 58 Rosseland mean opacity fit from
Valencia et al. (2013ApJ...775...10V 2013ApJ...775...10V)
Makefile 219 52 Makefile
test.csv 230 101 Example of output
--------------------------------------------------------------------------------
See also:
J/A+A/562/A133 : Analytical model for irradiated atmospheres (Parmentier+ 2014)
Acknowledgements:
Vivien Parmentier, vivien.parmentier(at)yahoo.fr
Licence :
This code is licensed under a Creative Commons
Attribution-NonCommercial-ShareAlike 3.0 Unported License (see
http://creativecommons.org/licenses/by-nc-sa/3.0/ for more details).
References:
Parmentier & Guillot, Paper I 2014A&A...562A.133P 2014A&A...562A.133P, Cat. J/A+A/562/A133
(End) Vivien Parmentier [OAC], Patricia Vannier [CDS] 28-Nov-2014