... | ... | @@ -37,16 +37,10 @@ Copy and edit the file _inputs/example.nml_, rename it _corot-4b.nml_. An extend |
|
|
```
|
|
|
5. Edit the stellar ("light source") parameters:
|
|
|
```text
|
|
|
add_light_source = True ! if True, add the light source
|
|
|
use_irradiation = False ! if True, use irradiation instead of range to calculate the light source spectrum
|
|
|
use_light_source_spectrum = True ! if True, use a spectrum for the light source instead of a black body
|
|
|
|
|
|
light_source_radius = 814e6 ! (m) radius of the light source
|
|
|
light_source_range = 13.5e9 ! (m) distance between the target and the light source
|
|
|
light_source_effective_temperature = 6190 ! (K) light source effective temperature
|
|
|
light_source_irradiation = 0 ! (W.m-2) light source irradiation
|
|
|
|
|
|
light_source_spectrum_file = 'spectrum_BTSettl_6200K_logg4.5_met0.dat' ! spectrum of the light sourcetarget
|
|
|
```
|
|
|
6. As a starting point, we will use a metallicity of 1 times the solar metallicity, no cloud, and a fixed eddy diffusion coefficient. Because of the effective temperature of the planet, TiO, VO and FeH are unlikely to have significant absorptions, so we will remove them in order to speed-up the calculations:
|
|
|
```text
|
... | ... | @@ -99,13 +93,13 @@ The figures should be in the _outputs/figures_ directory. |
|
|
|
|
|
The temperature profile figure (temperature_profile_corot-4b) should look like this:
|
|
|
|
|
|

|
|
|

|
|
|
|
|
|
The profile crosses the condensation curves of several species. It seems that clouds are likely to form on this planets.
|
|
|
|
|
|
The transmission spectrum should look like this:
|
|
|
|
|
|

|
|
|

|
|
|
|
|
|
This is nice, but the resolution is quite low.
|
|
|
|
... | ... | |