radis.phys package¶
Submodules¶
- radis.phys.air module
- radis.phys.blackbody module
- radis.phys.constants module
- radis.phys.convert module
J2K()
J2cm()
J2eV()
K2J()
K2cm()
K2eV()
atm2bar()
atm2torr()
bar2atm()
bar2torr()
cm2J()
cm2J_vaex()
cm2K()
cm2eV()
cm2hz()
cm2nm()
cm2nm_air()
dcm2dnm()
dcm2dnm_air()
dhz2dnm()
div_safe()
dnm2dcm()
dnm2dhz()
dnm_air2dcm()
eV2J()
eV2K()
eV2cm()
eV2nm()
hz2cm()
hz2nm()
nm2cm()
nm2eV()
nm2hz()
nm_air2cm()
torr2atm()
torr2bar()
zero2nan()
- radis.phys.morse module
- radis.phys.units module
- radis.phys.units_astropy module
Module contents¶
Physical constants and conversion.
- planck(lambda_, T, eps=1, unit='mW/cm2/sr/nm')[source]¶
Planck function for blackbody radiation.
\[\epsilon \frac{2h c^2}{{\lambda}^5} \frac{1}{\operatorname{exp}\left(\frac{h c}{\lambda k T}\right)-1}\]- Parameters:
λ (np.array (nm)) – wavelength
T (float (K)) – equilibrium temperature
eps (grey-body emissivity) – default 1
unit (output unit) – default ‘mW/sr/cm2/nm’
- Returns:
np.array – equilibrium radiance
- Return type:
(mW.sr-1.cm-2/nm)
See also
sPlanck()
,planck_wn()
- planck_wn(wavenum, T, eps=1, unit='mW/cm2/sr/cm-1')[source]¶
Planck function for blackbody radiation, wavenumber version.
\[\epsilon 2h c^2 {\nu}^3 \frac{1}{\operatorname{exp}\left(\frac{h c \nu}{k T}\right)-1}\]- Parameters:
wavenum (np.array (cm-1)) – wavenumber
T (float (K)) – equilibrium temperature
eps (grey-body emissivity) – default 1
unit (str) – output unit. Default ‘mW/sr/cm2/cm-1’
- Returns:
np.array – equilibrium radiance
- Return type:
default (mW/sr/cm2/cm-1)
See also
sPlanck()
,planck()
- sPlanck(wavenum_min=None, wavenum_max=None, wavelength_min=None, wavelength_max=None, T=None, eps=1, wstep=0.01, medium='air', **kwargs)[source]¶
Return a RADIS
Spectrum
object with blackbody radiation.It’s easier to plug in a
SerialSlabs()
line-of-sight than the Planck radiance calculated byplanck()
. And you don’t need to worry about units as they are handled internally.See
Spectrum
documentation for more information- Parameters:
wavenum_min / wavenum_max (():math:
cm^{-1}
)) – minimum / maximum wavenumber to be processed in \(cm^{-1}\).wavelength_min / wavelength_max ((\(nm\))) – minimum / maximum wavelength to be processed in \(nm\).
T (float (K)) – blackbody temperature
eps (float [0-1]) – blackbody emissivity. Default
1
- Other Parameters:
wstep (float (cm-1 or nm)) – wavespace step for calculation
**kwargs (other keyword inputs) – all are forwarded to spectrum conditions. For instance you can add a ‘path_length=1’ after all the other arguments
Examples
Generate Earth blackbody:
s = sPlanck(wavelength_min=3000, wavelength_max=50000, T=288, eps=1) s.plot()
Examples using sPlanck :
Blackbody radiationReferences
In wavelength:
\[\epsilon \frac{2h c^2}{{\lambda}^5} \frac{1}{\operatorname{exp}\left(\frac{h c}{\lambda k T}\right)-1}\]In wavenumber:
\[\epsilon 2h c^2 {\nu}^3 \frac{1}{\operatorname{exp}\left(\frac{h c \nu}{k T}\right)-1}\]See also