def test_issue_4(self):
"""
uibei shouldn't fail when energy_lo == chem_potential
"""
try:
ibei.uibei(2, 1., 300., 1.)
except:
self.fail("uibei fails when energy_lo == chem_potential")
def test_issue_2_uibei(self):
"""
Refactor of issue 2 focusing on uibei
"""
try:
ibei.uibei(2, bandgap, temp_sun, 1.2)
except:
self.fail("Error raised with arguments.")
def photon_flux(self):
"""
Number of photons per unit time per unit area
:returns: `astropy.units.Quantity` in units of :math:`s^{-1} cm^{-2}`.
"""
photon_flux = self.emissivity * uibei(2, 0, self.temp, 0)
return photon_flux.to("1/(s*cm2)")
def photon_flux(self):
"""
Number of photons per unit time per unit area
:returns: `astropy.units.Quantity` in units of :math:`s^{-1} cm^{-2}`.
"""
photon_flux = self.emissivity * uibei(2, self.bandgap, self.temp, 0)
return photon_flux.to("1/(s*cm2)")
def calc_power_density(self):
"""
Solar cell power density
The output power density is calculated according to DeVos's :cite:`9780198513926` Eq. 6.4. Note that this expression assumes fully concentrated sunlight and is therefore not completely general.
This method returns values of type :class:`astropy.units.Quantity` with units of [W m^-2].
"""
electron_energy = constants.e.si * self.voltage
if self.bandgap == 0:
solar_flux = units.Quantity(0., "1/(m2*s)")
solar_cell_flux = units.Quantity(0., "1/(m2*s)")
else:
solar_flux = uibei(2, self.bandgap, self.temp_sun, 0)
solar_cell_flux = uibei(2, self.bandgap, self.temp_planet, electron_energy)
power_density = electron_energy * (solar_flux - solar_cell_flux)
return power_density.to("W/m^2")
def calc_power_density(self):
"""
Solar cell power density
The output power density is calculated according to a slight modification of Shockley & Queisser's :cite:`10.1063/1.1736034` Eq. 2.4. This method returns values of type :class:`astropy.units.Quantity` with units of [W m^-2].
"""
if self.bandgap == 0:
solar_flux = units.Quantity(0., "1/(m2*s)")
else:
solar_flux = uibei(2, self.bandgap, self.temp_sun, 0)
power_density = self.bandgap * solar_flux
return power_density.to("W/m^2")
def photon_energy_flux(self):
"""
Energy flux emitted by Stefan-Boltzmann radiation
The energy flux (or power density) of Stefan-Boltzmann photons is given by
.. math::
j = \\frac{2 \pi^{5} k^{4}}{15 c^{2} h^{3}} T^{4}
:returns: `astropy.units.Quantity` in units of :math:`W cm^{-2}`.
"""
energy_flux = self.emissivity * uibei(3, 0, self.temp, 0)
return energy_flux.to("W/cm2")
def photon_energy_flux(self):
"""
Energy flux emitted by Stefan-Boltzmann radiation
The energy flux (or power density) of Stefan-Boltzmann photons is given by
.. math::
j = \\frac{2 \pi^{5} k^{4}}{15 c^{2} h^{3}} T^{4}
:returns: `astropy.units.Quantity` in units of :math:`W cm^{-2}`.
"""
energy_flux = self.emissivity * uibei(3, self.bandgap, self.temp, 0)
return energy_flux.to("W/cm2")
def test_issue_31(self):
"""
Passing `energy_lo=0` with `chem_potential=0` should yield nonzero result
"""
energy_flux = ibei.uibei(3, 0., 300., 0.)
self.assertGreater(energy_flux, 0)
