from __future__ import annotations
import numpy as np
import sasktran2 as sk
from sasktran2.constants import K_BOLTZMANN
from sasktran2.database.web import StandardDatabase
from . import database, refraction # noqa: F401
from .aerline import AERLineAbsorber # noqa: F401
from .henyey import HenyeyGreenstein # noqa: F401
from .hitran import (
HITRANAbsorber, # noqa: F401
)
from .mie import Mie # noqa: F401
from .xsec_absorber import ( # noqa: F401
IOGeisa,
O2LymanAlpha,
O2SchumannRunge,
OClOGeisa,
XsecAbsorber,
)
[docs]
class O3DBM(database.OpticalDatabaseGenericAbsorber):
[docs]
def __init__(self) -> None:
"""
Tabulated high resolution cross-sections of O3 measured by Daumont, Brion and Malicet in the early 1990's [1].
The wavelength range slightly varies with temperature but covers the entire UV to NIR region, from 194.50 nm to
830.00 nm at 0.01 to 0.02 nm resolution. The cross-section data were collected at 0.01-0.02 nm resolution and
each wavelength/cross-section table varies in size from 22,052 to 63,501 entries. The data consists of 5 tables
of wavelength versus cross-section for 5 temperatures.
Notes
-----
Temerature Range
Measurements are provided at 5 temperatures covering typical stratospheric and
tropospheric conditions:
| 218 K
| 228 K
| 243 K
| 273 K
| 295 K
Wavelength Range
The wavelength range of each temperature table is slightly different and is given below.
Note that most of the temperature variation occurs in the Huggins band
between 315 and 360 nm:
| 218K -> 194.50nm to 650.01nm
| 228K -> 194.50nm to 520.01nm
| 243K -> 194.50nm to 519.01nm
| 273K -> 299.50nm to 520.01nm
| 295K -> 195.00nm to 830.00nm
We looked into temperature interpolation and while DBM suggest that a quadratic interpolation scheme [3] they do
not indicate an explicit technique. We tested several quadratic fitting routines and found that a truncated linear
fit in temperature was visually more appealing than any of the quadratic fits and had none of the undesirable
artifacts (excessive curvature etc.) that naturally arise with quadratic curve fitting. Consequently this object
uses a truncated linear fit in temperature.
Data Source
These data are an exact replication of the data files:
| O3_CRS_BDM_218K.dat
| O3_CRS_BDM_228K.dat
| O3_CRS_BDM_243K.dat
| O3_CRS_BDM_273K.dat
| O3_CRS_BDM_295K.dat
Data is from the IGACO site, http://igaco-o3.fmi.fi/ACSO/cross_sections.html. The files were copied on
July 16-July 25 2012.
References
----------
.. [1] Daumont, D., et al. "Ozone UV spectroscopy I: Absorption cross-sections at room temperature."
Journal of Atmospheric Chemistry 15.2 (1992): 145-155.
.. [2] Brion, J., et al. "High-resolution laboratory absorption cross section of O3. Temperature effect."
Chemical physics letters 213.5 - 6(1993): 610-612.
.. [3] Malicet, J., et al. "Ozone UV spectroscopy. II. Absorption cross-sections and temperature dependence."
Journal of Atmospheric Chemistry 21.3 (1995): 263-273.
.. [4] Brion, J., et al. "Absorption spectra measurements for the ozone molecule in the 350-830 nm region."
Journal of Atmospheric Chemistry 30.2 (1998): 291-299.
Raises
------
OSError
If the file could not be found
"""
dbm_file = StandardDatabase().path("cross_sections/o3/dbm.nc")
if dbm_file.exists():
super().__init__(dbm_file)
else:
msg = "Could not find DBM file"
raise OSError(msg)
[docs]
class NO2Vandaele(database.OpticalDatabaseGenericAbsorber):
[docs]
def __init__(self) -> None:
"""
Calculates the absorption cross section of NO2 molecules from 230 nm to 1000 nm at 220 K to 294 K following [1]
.. [1] Vandaele, Ann Carine, et al. "Measurements of the NO2 absorption cross-section from 42 000 cm-1 to
10 000 cm-1 (238-1000 nm) at 220 K and 294 K." Journal of Quantitative Spectroscopy and Radiative Transfer
59.3-5 (1998): 171-184.
Raises
------
OSError
If the Vandaele file cannot be found
"""
v_file = StandardDatabase().path("cross_sections/no2/vandaele.nc")
if v_file.exists():
super().__init__(v_file)
else:
msg = "Could not find Vandaele file"
raise OSError(msg)
[docs]
class HITRANUV(database.OpticalDatabaseGenericAbsorber):
[docs]
def __init__(self, name: str, version: str = "2022") -> None:
"""
HITRAN UV cross-sections for a given constituent. The constituent must be one of the following:
["O3", "NO2", "BrO", "SO2"]
These are the files that you obtain from the HITRAN website when selecting UV cross sections.
Note that usually these are not very good, and you should use a specific database for each constituent instead
such as O3DBM. The HITRAN UV cross sections are only provided for convenience.
Specific Issues
O3
We have noticed the Ozone cross sections are unreasonably large in the region < 310 nm, and does not match the source data.
We do not recommend using this.
NO2
Even though the HITRAN database specifically says all cross sections are given in vacuum wavenumbers, this one
seems to be specified in air wavenumbers. We have converted it to vacuum wavenumbers manually. After doing so
it matches the Vandaele source files relatively well.
Parameters
----------
name : str
Constituent
version : str, optional
HITRAN version number, currently only "2022" is supported, by default "2022"
Raises
------
OSError
If the databases are not installed
"""
data_file = StandardDatabase().path(f"cross_sections/{name}/hitran{version}.nc")
if data_file.exists():
super().__init__(data_file)
else:
msg = f"Could not find HITRAN UV database for {name} at {data_file}"
raise OSError(msg)
[docs]
class HITRANTabulated(database.OpticalDatabaseGenericAbsorber):
[docs]
def __init__(self, name: str, res="01nm") -> None:
"""
Loads in a database tabulated from HITRAN line entries as a function of pressure/temperature that have been
reduced to a given resolution.
This requires the extended databases to be downloaded, e.g. by running sk.appconfig.download_extended_databases()
Currently supported species and resolutions are:
| H2O : 01nm
| O2 : 01nm
Parameters
----------
name : str
Species name
res : str, optional
Resolution of the database to load in, by default "01nm"
Raises
------
OSError
If the specified file cannot be found
"""
data_file = sk.appconfig.database_root().joinpath(
f"cross_sections/{name.lower()}/hitran_{res}_res.nc"
)
if data_file.exists():
super().__init__(data_file)
else:
msg = f"Could not find HITRAN database for {name} at {data_file}"
raise OSError(msg)
[docs]
class HITRANCollision(database.OpticalDatabaseGenericAbsorber):
[docs]
def __init__(self, name: str) -> None:
"""
Loads collision induced absorption (CIA) cross sections compiled from data found at https://hitran.org/cia/.
This requires the extended databases to be downloaded, e.g. by running sk.appconfig.download_extended_databases()
Currently supported species are:
| O2O2
Parameters
----------
name : str
Species name
"""
data_file = StandardDatabase().path(
f"cross_sections/{name.lower()}/hitran_cia.nc"
)
if data_file.exists():
super().__init__(data_file)
else:
msg = f"Could not find HITRAN CIA database for {name} at {data_file}"
raise OSError(msg)
def pressure_temperature_to_numberdensity(
pressure_pa: np.array, temperature_k: np.array, include_derivatives=False
) -> np.array:
"""
Converts pressure and temperature to number density using the ideal gas law
Parameters
----------
pressure_pa : np.array
Pressure in [Pa]
temperature_k : np.array
Temperature in [K]
include_derivatives: bool, optional
If set to true, the derivative of the number density with respect to pressure and temperature will be returned
alongside the numberdensity. The return signature is then np.array, np.array, np.array
Returns
-------
np.array, if include_derivatives is False
Number density in [molecules / m^3]
np.array, np.array, np.array if include_derivatives is True
Number density, dN/dP, dN/dT in [molecules / m^3], [molecules / m^3 / Pa], [molecules / m^3 / K]
"""
# Ideal gas law is PV = N k T
# Or (N/V) = P / (k T)
N = pressure_pa / (K_BOLTZMANN * temperature_k)
if not include_derivatives:
return N
dN_dP = 1 / (K_BOLTZMANN * temperature_k)
dN_dT = -pressure_pa / (K_BOLTZMANN * temperature_k**2)
return N, dN_dP, dN_dT
def air_wavelength_to_vacuum_wavelength(wavelength_nm: np.array) -> np.array:
"""
Converts wavelength specified in Air at STP to wavelengths at vacuum
Parameters
----------
wavelength_nm : np.array
Wavelength in air at STP
Returns
-------
np.array
Vacuum wavelengths
"""
s = 1e4 / (wavelength_nm * 10) # Convert to angstroms
refac_index = (
1
+ 0.00008336624212083
+ 0.02408926869968 / (130.1065924522 - s**2)
+ 0.0001599740894897 / (38.92568793293 - s**2)
)
return wavelength_nm * refac_index
def vacuum_wavelength_to_air_wavelength(wavelength_nm: np.array) -> np.array:
"""
Converts wavelength specified in vacuum to wavelengths at air at STP
Parameters
----------
wavelength_nm : np.array
Wavelengths in vacuum
Returns
-------
np.array
Wavelengths in air at STP
"""
s = 1e4 / (wavelength_nm * 10) # Convert to angstroms
n = 1 + 0.0000834254 + 0.02406147 / (130 - s**2) + 0.00015998 / (38.9 - s**2)
return wavelength_nm / n
