def test_units(verbose=True, *args, **kwargs):
# Test unit-ware arrays
# RADIS pint-aware array
a = uarray(np.linspace(10, 100, 10), 'Td')
res = Q_(np.linspace(1e-16, 1e-15, 10), 'V * cm^2') # pint definition
assert (np.round(np.array(a.to('V * cm^2')) - np.array(res), 5)
== np.zeros_like(res)).all()
# b = (print(a.to('V * cm^2'))==print(res))
# Test conversion
convtable = [
(500, 'nm', 0.5, 'µm'),
(1, 'erg/s', 1e-7, 'W'),
(1, 'm2', 10000, 'cm2')
]
for a, f, r, t in convtable:
cr = conv2(a, f, t)
if verbose:
print(('{0} {1} = {2} {3}'.format(a, f, cr, t)))
assert isclose(cr, r)
# Ensures that an error is raised if units with angles are converted
# (mathematically correct because angles are dimensionless, but prone
# to user errors)
from radis.phys.units import DimensionalityError
with pytest.raises(DimensionalityError):
conv2(1, 'mW/cm2/sr/nm', 'mW/cm2/nm')
return True
def test_units(verbose=True, *args, **kwargs):
# Test unit-ware arrays
# RADIS pint-aware array
# b = (print(a.to('V * cm^2'))==print(res))
# Test conversion
convtable = [
(500, "nm", 0.5, "µm"),
(1, "erg/s", 1e-7, "W"),
(1, "m**2", 10000, "cm**2"),
]
for a, f, r, t in convtable:
cr = conv2(a, f, t)
if verbose:
print(("{0} {1} = {2} {3}".format(a, f, cr, t)))
assert isclose(cr, r)
# Ensures that an error is raised if units with angles are converted
# (mathematically correct because angles are dimensionless, but prone
# to user errors)
assert not is_homogeneous("mW/cm2/sr/nm", "mW/cm2/nm")
with pytest.raises(TypeError):
conv2(1, "mW/cm**2/sr/nm", "mW/cm**2/nm")
return True
def planck_wn(wavenum, T, eps=1, unit="mW/sr/cm2/cm-1"):
"""Planck function for blackbody radiation, wavenumber version.
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
-------
planck: np.array default (mW/sr/cm2/cm-1)
equilibrium radiance
"""
k = k_b_CGS
h = h_CGS
c = c_CGS
iplanck = (eps * (2 * h * c**2 * wavenum**3) * 1 / (exp(h * c * wavenum /
(k * T)) - 1))
# iplanck in erg/s/sr/cm2/cm-1
iplanck *= 1e-4 # erg/s/sr/cm2/cm-1 > mW/sr/cm^2/cm-1
if Q_(unit) != Q_("mW/sr/cm2/cm-1"):
iplanck = conv2(iplanck, "mW/sr/cm2/cm-1", unit)
return iplanck
def planck(lmbda, T, eps=1, unit="mW/sr/cm2/nm"):
"""Planck function for blackbody radiation.
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
-------
planck: np.array (mW.sr-1.cm-2/nm)
equilibrium radiance
"""
k = k_b
lbd = lmbda * 1e-9
iplanck = (eps * (2 * h * c**2 / lbd**5) * 1 /
(exp(h * c / (lbd * k * T)) - 1)) # S.I (W.sr-1.m-3)
iplanck *= 1e-10 # W.sr-1.m-3 >>> mW.sr-1.cm-2.nm-1
if Q_(unit) != Q_("mW/sr/cm2/nm"):
iplanck = conv2(iplanck, "mW/sr/cm2/nm", unit)
return iplanck
def test_units(verbose=True, *args, **kwargs):
# Test unit-ware arrays
a = uarray(np.linspace(10, 100, 10), 'Td') # RADIS pint-aware array
res = Q_(np.linspace(1e-16, 1e-15, 10), 'V * cm^2') # pint definition
assert (np.round(np.array(a.to('V * cm^2')) - np.array(res),
5) == np.zeros_like(res)).all()
# b = (print(a.to('V * cm^2'))==print(res))
# Test conversion
convtable = [(500, 'nm', 0.5, 'µm'), (1, 'erg/s', 1e-7, 'W'),
(1, 'm2', 10000, 'cm2')]
for a, f, r, t in convtable:
cr = conv2(a, f, t)
if verbose: print(('{0} {1} = {2} {3}'.format(a, f, cr, t)))
assert isclose(cr, r)
return True
def planck_wn(wavenum, T, eps=1, unit="mW/sr/cm2/cm-1"):
r"""Planck function for blackbody radiation, wavenumber version.
.. math::
\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 : default (mW/sr/cm2/cm-1)
equilibrium radiance
See Also
--------
:py:func:`~radis.blackbody.sPlanck`, :py:func:`~radis.phys.blackbody.planck`
"""
k = k_b_CGS
h = h_CGS
c = c_CGS
iplanck = (
eps
* (2 * h * c ** 2 * wavenum ** 3)
* (1 / (exp(h * c * wavenum / (k * T)) - 1))
)
# iplanck in erg/s/sr/cm2/cm-1
iplanck *= 1e-4 # erg/s/sr/cm2/cm-1 > mW/sr/cm^2/cm-1
if Q_(unit) != Q_("mW/sr/cm2/cm-1"):
iplanck = conv2(iplanck, "mW/sr/cm2/cm-1", unit)
return iplanck
def planck(lmbda, T, eps=1, unit="mW/sr/cm2/nm"):
r"""Planck function for blackbody radiation.
.. math::
\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 : (mW.sr-1.cm-2/nm)
equilibrium radiance
See Also
--------
:py:func:`~radis.blackbody.sPlanck`, :py:func:`~radis.phys.blackbody.planck_wn`
"""
k = k_b
lbd = lmbda * 1e-9
iplanck = (
eps * (2 * h * c ** 2 / lbd ** 5) * (1 / (exp(h * c / (lbd * k * T)) - 1))
) # S.I (W.sr-1.m-3)
iplanck *= 1e-10 # W.sr-1.m-3 >>> mW.sr-1.cm-2.nm-1
if Q_(unit) != Q_("mW/sr/cm2/nm"):
iplanck = conv2(iplanck, "mW/sr/cm2/nm", unit)
return iplanck
