irfpy.util.solarspectra
¶
Solar spectrum models at the Earth orbit
Code author: Yoshifumi Futaana

Black body assumption of the Sun. 

Black body assumption with constant FUV (<~100 nm) modification 

Air mass 0 model (at extraterrestorial) under ASTM E490. 
Solar spectrum models at the Earth orbit (1 AU).
See also irfpy.util.planck
.
 class irfpy.util.solarspectra.BlackBody(temperature=5778.0)[source]¶
Bases:
object
Black body assumption of the Sun.
Sun is proxied by a black body with tempereature 5778 K.
Using the planck’s formula (see
irfpy.util.planck.BlackBodyMksa
) the spectrum at the Sun, i.e. power by area by wavelength [W / m2 / sr/ m], is immediately known as \(B(\lambda, T)\). This is implemented inirfpy.util.planck
.The total spectral power is the integral over the Sun surface area and the emission angle (in solid angle). As isotropic emission is assumed, the solid angle integral can be done
\[\int{\cos\theta d\Omega} = \int_0^{2\pi}d\phi\int_0^{\pi/2}\cos\theta\sin\theta d\theta = \pi\]The \(\cos\theta\) appears from the inner product of the flux and the surface area. See also how to derive StefanBoltzmann law. Same calculation is done.
Anyway, the total spectral power, in the unit of [W / m], is
\[F(\lambda, T) = \pi B(\lambda, T) \times 4\pi Rs^2\]Here
Rs
is the radius of the Sun.Consider a unit area at the Earth’s orbit. The spectral power through the area is, as the emission is isotropic, calculated by multiplying the fraction of the area to the sphare surface at 1AU, namely,
\[u(\lambda, T) = F(\lambda, T) \times \frac{1}{4\pi a^2}\]where
a
is 1AU. The unit ofu
is [W / m2 / m].In summary, the spectrum power at the Earth orbit,
u
[W / m2 / m] is\[u(\lambda, T) = \pi \frac{Rs^2}{a^2} B(\lambda, T)\]Substituting Rs=695500 km and a=149597871 km,
\[u(\lambda, T) = 6.8687\times10^5 B(\lambda, T)\] name¶
Name of the model
 spectral_irradiance(wavelength)[source]¶
Return the spectral irradiance (W / m2 / m).
Return the spectral irradiance, in the unit of W / m2 / m.
 Parameters
wavelength – Wavelength in m.
 Returns
Spectral irradiance in W / m2 / m
>>> sun = BlackBody(5800) # 5800 K blackbody approx. >>> irr500nm = sun.spectral_irradiance(500e9) >>> print('%.3e' % irr500nm) 1.846e+09
 photon_flux(wavelength)[source]¶
Return the photon’s differential flux (# / m2 / s / m).
The spectral irradiance, u [W / m2 / m = J / m2 / s / m], can be converted to the photon flux.
A photon with wavelength, \(\lambda\), will have the energy \(E = hc/\lambda\). Thus, the number of photons through a unit area per unit time is \(F = u / E\).
>>> sun = BlackBody(5800) >>> fph = sun.photon_flux(500e9) # in /m2 /s /m >>> fph = fph / 1e9 # in m2 /s /nm >>> print('%.3e' % fph) 4.648e+18
 class irfpy.util.solarspectra.BlackBodyModFuv(*args, **kwds)[source]¶
Bases:
irfpy.util.solarspectra.BlackBody
Black body assumption with constant FUV (<~100 nm) modification
 name¶
Name of the model
 class irfpy.util.solarspectra.AM0[source]¶
Bases:
object
Air mass 0 model (at extraterrestorial) under ASTM E490.
>>> am0 = AM0() >>> irr = am0.spectral_irradiance(500e9) >>> print('%.3e' % irr) 1.914e+09 >>> fph = am0.photon_flux(np.array([500e9, 1000e9])) >>> print('%.3e %.3e' % (fph[0] / 1e9, fph[1] / 1e9)) # in m2 /nm /s 4.816e+18 3.765e+18
 logger = <Logger irfpy.util.solarspectra.AM0 (DEBUG)>¶
 irradfunc¶
The irradiance function from wavelength (nm) to irradiance (W/m2/nm)