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Python constants.h方法代碼示例

本文整理匯總了Python中scipy.constants.h方法的典型用法代碼示例。如果您正苦於以下問題:Python constants.h方法的具體用法?Python constants.h怎麽用?Python constants.h使用的例子?那麽, 這裏精選的方法代碼示例或許可以為您提供幫助。您也可以進一步了解該方法所在scipy.constants的用法示例。


在下文中一共展示了constants.h方法的15個代碼示例,這些例子默認根據受歡迎程度排序。您可以為喜歡或者感覺有用的代碼點讚,您的評價將有助於係統推薦出更棒的Python代碼示例。

示例1: population

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def population(self, Mole, Temp):
        """Calculate population for each level at given temperature"""
        RoTemp = np.reshape(Temp*1., (Temp.size, 1))
        Qr = self.weighti*np.exp(-(self.e_cm1*100*c*h)/(k*RoTemp))
        # RoPr = Qr/Ntotal  # This is for all transitions
        RoPr = Qr/(Qr.sum(axis=1).reshape(RoTemp.size, 1))  # only given trans.
        linet = []
        for xx in range(self.nt):
            gdu, gdl = self.weighti[self.tran_tag[xx][1:].astype(int)]
            _up = int(self.tran_tag[xx][1])
            _low = int(self.tran_tag[xx][2])
            Aei = self.ai[_up, _low]
            line_const = (c*10**2)**2*Aei*(gdu/gdl)*1.e-6*1.e14 /\
                         (8.*np.pi*(self.freq_array[xx]*1.e9)**2)
            # Hz->MHz,cm^2 ->nm^2
            # W = C.h*C.c*E_cm1[_low]*100.  # energy level above ground state
            "This is the function of calculating H2O intensity"
            line = (1.-np.exp(-h*(self.freq_array[xx]*1.e9) /
                              k/RoTemp))*line_const
            linet.append(line[:, 0]*RoPr[:, _low])  # line intensity non-LTE
        Ni_LTE = Mole.reshape((Mole.size, 1))*RoPr  # *0.75  # orth para ratio
        Ite_pop = [[Ni_LTE[i].reshape((self.ni, 1))] for i in range(Mole.size)]
        return Ite_pop

#import numba 
開發者ID:atmtools,項目名稱:typhon,代碼行數:27,代碼來源:__init__.py

示例2: test_tlcorrection

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def test_tlcorrection(self):
        # testing long correction function
        x_for_long = np.array([20.,21.,22.,23.,24.,25.])
        y_for_long = np.array([1.0,1.0,1.0,1.0,1.0,1.0])

        nu0 = 1.0/(514.532)*1e9 #laser wavenumber at 514.532
        nu = 100.0*x_for_long # cm-1 to m-1
        T = 23.0+273.15 # the temperature in K

        x_long,long_res,eselong = rp.tlcorrection(x_for_long, y_for_long,23.0,514.532,correction = 'long',normalisation='area') # using the function
        t0 = nu0**3.0*nu/((nu0-nu)**4)
        t1= 1.0 - np.exp(-h*c*nu/(k*T)) # c in m/s  : t1 dimensionless
        long_calc= y_for_long*t0*t1 # pour les y
        long_calc = long_calc/np.trapz(long_calc,x_for_long) # area normalisation

        np.testing.assert_equal(long_res,long_calc)
        np.testing.assert_equal(x_for_long,x_long)

        x_long,long_res,eselong = rp.tlcorrection(x_for_long, y_for_long,23.0,514.532,correction = 'long',normalisation='no') # using the function
        t0 = nu0**3.0*nu/((nu0-nu)**4)
        t1= 1.0 - np.exp(-h*c*nu/(k*T)) # c in m/s  : t1 dimensionless
        long_calc= y_for_long*t0*t1 # pour les y

        np.testing.assert_equal(long_res,long_calc)
        np.testing.assert_equal(x_for_long,x_long) 
開發者ID:charlesll,項目名稱:rampy,代碼行數:27,代碼來源:test_tlcorrection.py

示例3: Responsivity

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def Responsivity(wavelength, quantumEffic):
    """
    Responsivity quantifies the amount of output seen per watt of radiant
    optical power input [1]. But, for this application it is interesting to
    define spectral responsivity that is the output per watt of monochromatic
    radiation.

    The model used here is based on Equations 7.114 in Dereniak's book.

    Args:
        | wavelength: spectral variable [m]
        | quantumEffic: spectral quantum efficiency

    Returns:
        | responsivity in [A/W]
    """

    return (const.e * wavelength * quantumEffic) / (const.h * const.c)


################################################################################
# 
開發者ID:NelisW,項目名稱:pyradi,代碼行數:24,代碼來源:rydetector.py

示例4: plotSpectre

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def plotSpectre(transitions, eneval, spectre):
    """ plot the UV-visible spectrum using matplotlib. Absissa are converted in nm. """

    # lambda in nm
    lambdaval = [cst.h * cst.c / (val * cst.e) * 1.e9 for val in eneval]

    # plot gaussian spectra
    plt.plot(lambdaval, spectre, "r-", label = "spectre")

    # plot transitions
    plt.vlines([val[1] for val in transitions], \
               0., \
               [val[2] for val in transitions], \
               color = "blue", \
               label = "transitions" )

    plt.xlabel("lambda   /   nm")
    plt.ylabel("Arbitrary unit")
    plt.title("UV-visible spectra")
    plt.grid()
    plt.legend(fancybox = True, shadow = True)
    plt.show() 
開發者ID:gVallverdu,項目名稱:myScripts,代碼行數:24,代碼來源:spectre.py

示例5: get_electron_wavelength

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def get_electron_wavelength(accelerating_voltage):
    """Calculates the (relativistic) electron wavelength in Angstroms for a
    given accelerating voltage in kV.

    Parameters
    ----------
    accelerating_voltage : float or 'inf'
        The accelerating voltage in kV. Values `numpy.inf` and 'inf' are
        also accepted.

    Returns
    -------
    wavelength : float
        The relativistic electron wavelength in Angstroms.

    """
    if accelerating_voltage in (np.inf, "inf"):
        return 0
    E = accelerating_voltage * 1e3
    wavelength = (
        h / math.sqrt(2 * m_e * e * E * (1 + (e / (2 * m_e * c * c)) * E)) * 1e10
    )
    return wavelength 
開發者ID:pyxem,項目名稱:diffsims,代碼行數:25,代碼來源:sim_utils.py

示例6: PopuSource

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def PopuSource(LowerPop, UpperPop, LowerDeg, UpperDeg, Freq_c):
    sij = (2.*h*Freq_c**3)/(c**2*(LowerPop*UpperDeg/UpperPop/LowerDeg-1.))
    return sij 
開發者ID:atmtools,項目名稱:typhon,代碼行數:5,代碼來源:source_function.py

示例7: Bv_T

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def Bv_T(Freq, T):
    # brbr = 1  # .e7*1.e-4
    Bv_out = 2.*h*Freq**3/c**2/(np.exp(h*Freq/k/T)-1.)
    return Bv_out 
開發者ID:atmtools,項目名稱:typhon,代碼行數:6,代碼來源:source_function.py

示例8: basic

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def basic(LowerPop, UpperPop, Blu, Bul, Freq):
    u"""
    calculate absorption coefficient.\n
    Freq should be Hz
    """
    _const = h*Freq/4./np.pi
    return (LowerPop*Blu - UpperPop*Bul)*_const 
開發者ID:atmtools,項目名稱:typhon,代碼行數:9,代碼來源:abscoeff.py

示例9: calc_abscoeff

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def calc_abscoeff(tran, itera, alt=None):
    _up, _low = Tran_tag[tran][1:].astype(int)
    _v0 = Freqi[_up, _low]*1.e9
    _const = C.h*_v0/4./N.pi
    if alt is None:
        lowerPop = N.array(Ite_pop)[alt][itera][_low][0]
        upperPop = N.array(Ite_pop)[alt][itera][_up][0]
    else:
        lowerPop = N.array(Ite_pop)[:, itera, _low, 0]
        upperPop = N.array(Ite_pop)[:, itera, _up, 0]
    BLU = Blu[_up, _low]
    BUL = Bul[_up, _low]
    # AUL = Ai[_up, _low]
    return (lowerPop*BLU - upperPop*BUL)*_const 
開發者ID:atmtools,項目名稱:typhon,代碼行數:16,代碼來源:abscoeff.py

示例10: test_twomode

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def test_twomode(self):
        """Test if function returns two-mode squeezing parameters that correctly reconstruct the
        input normal mode frequencies."""
        w = -k * self.T / (0.5 * h * c * 100) * np.log(np.tanh(self.t))
        assert np.allclose(w, self.w) 
開發者ID:XanaduAI,項目名稱:strawberryfields,代碼行數:7,代碼來源:test_vibronic.py

示例11: planck

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def planck(lam, T):
    """ Returns the spectral radiance of a black body at temperature T.

    Returns the spectral radiance, B(lam, T), in W.sr-1.m-2 of a black body
    at temperature T (in K) at a wavelength lam (in nm), using Planck's law.

    """

    lam_m = lam / 1.e9
    fac = h*c/lam_m/k/T
    B = 2*h*c**2/lam_m**5 / (np.exp(fac) - 1)
    return B 
開發者ID:mjhoptics,項目名稱:ray-optics,代碼行數:14,代碼來源:colour_system.py

示例12: Absorption

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def Absorption(wavelength, Eg, tempDet, a0, a0p):
    """
    Calculate the spectral absorption coefficient
    for a semiconductor material with given material values.

    The model used here is based on Equations 3.5, 3.6 in Dereniaks book.

    Args:
        | wavelength: spectral variable [m]
        | Eg: bandgap energy [Ev]
        | tempDet: detector's temperature in [K]
        | a0: absorption coefficient [m-1] (Dereniak Eq 3.5 & 3.6)
        | a0p:  absorption coefficient in [m-1] (Dereniak Eq 3.5 & 3.6)

    Returns:
        | absorption: spectral absorption coefficient in [m-1]
    """

    #frequency/wavelength expressed as energy in Ev
    E = const.h * const.c / (wavelength * const.e )

    # the np.abs() in the following code is to prevent nan and inf values
    # the effect of the abs() is corrected further down when we select
    # only the appropriate values based on E >= Eg and E < Eg

    # Absorption coef - eq. 3.5- Dereniak
    a35 = (a0 * np.sqrt(np.abs(E - Eg))) + a0p
    # Absorption coef - eq. 3.6- Dereniak
    a36 = a0p * np.exp((- np.abs(E - Eg)) / (const.k * tempDet))
    absorption = a35 * (E >= Eg) + a36 * (E < Eg)

    return absorption

################################################################################
# 
開發者ID:NelisW,項目名稱:pyradi,代碼行數:37,代碼來源:rydetector.py

示例13: deeStarPeak

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def deeStarPeak(wavelength,temperature,eta,halfApexAngle):
        i = 0
        for wlc in wavelength:
            wl =  np.linspace(wlc/100, wlc, 1000).reshape(-1, 1)
            LbackLambda = ryplanck.planck(wl,temperature, type='ql')/np.pi
            Lback = np.trapz(LbackLambda.reshape(-1, 1),wl, axis=0)[0]
            Eback = Lback * np.pi * (np.sin(halfApexAngle)) ** 2
            # funny construct is to prevent divide by zero
            tempvar = np.sqrt(eta/(Eback+(Eback==0))) * (Eback!=0) + 0 * (Eback==0)
            dstarwlc[i] = 1e-6 * wlc * tempvar/(const.h * const.c * np.sqrt(2))
            #print(Eback)
            i = i + 1
        return dstarwlc * 100. # to get cm units 
開發者ID:NelisW,項目名稱:pyradi,代碼行數:15,代碼來源:rydetector.py

示例14: __init__

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def __init__(self):
        """ Precalculate the Planck function constants.

        Reference: http://www.spectralcalc.com/blackbody/appendixC.html
        """

        import scipy.optimize

        self.c1em = 2 * np.pi * const.h * const.c * const.c
        self.c1el = self.c1em * (1.0e6)**(5-1) # 5 for lambda power and -1 for density
        self.c1en = self.c1em * (100)**3 * 100 # 3 for wavenumber, 1 for density
        self.c1ef = 2 * np.pi * const.h / (const.c * const.c)

        self.c1qm = 2 * np.pi * const.c
        self.c1ql = self.c1qm * (1.0e6)**(4-1) # 5 for lambda power and -1 for density
        self.c1qn = self.c1qm * (100)**2 * 100 # 2 for wavenumber, 1 for density
        self.c1nf = 2 * np.pi  / (const.c * const.c)

        self.c2m = const.h * const.c / const.k
        self.c2l = self.c2m * 1.0e6 # 1 for wavelength density
        self.c2n = self.c2m * 1.0e2 # 1 for cm-1 density
        self.c2f = const.h / const.k

        self.sigmae = const.sigma
        self.zeta3 = 1.2020569031595942853
        self.sigmaq = 4 * np.pi * self.zeta3 * const.k ** 3 \
               / (const.h ** 3 * const.c ** 2)

        self.a2 = scipy.optimize.brentq(self.an, 1, 2, (2) )
        self.a3 = scipy.optimize.brentq(self.an, 2, 3, (3) )
        self.a4 = scipy.optimize.brentq(self.an, 3.5, 4, (4) )
        self.a5 = scipy.optimize.brentq(self.an, 4.5, 5, (5) )

        self.wel = 1e6 * const.h * const.c /(const.k * self.a5)
        self.wql = 1e6 * const.h * const.c /(const.k * self.a4)
        self.wen = self.a3 * const.k /(100 * const.h * const.c )
        self.wqn = self.a2 * const.k /(100 * const.h * const.c )
        self.wef = self.a3 * const.k /(const.h )
        self.wqf = self.a2 * const.k /(const.h ) 
開發者ID:NelisW,項目名稱:pyradi,代碼行數:41,代碼來源:ryplanck.py

示例15: calcLuxEquivalent

# 需要導入模塊: from scipy import constants [as 別名]
# 或者: from scipy.constants import h [as 別名]
def calcLuxEquivalent(wavelength,rad_min,rad_dynrange,units):
    """Calc the interpolation function between lux and photon rate radiance

    Assuming single wavelength colour, the specified wavelength value is used to 
    calculate the lux equivalent lux image for the radiance input range.

    Args:
        | wavelength (np.array): wavelength vector
        | sysresp (np.array): system response spectral vector
        | rad_min (float): minimum photon rate radiance lookup table 
        | rad_dynrange (float): maximum photon rate radiance in lookup table 
        | units (string): input radiance units q/s or W

    Returns:
        | interpolation function

    Raises:
        | No exception is raised.

    Author: CJ Willers
    """
    if 'q' in units:
        conversion = wavelength / (const.h * const.c)
    else:
        conversion = 1.

    Wm2tolux = 683 * 1.019 * np.exp(-285.51 * (wavelength*1e6 - 0.5591)**2)
    # convert from q/s to W
    rad_minW = rad_min / conversion
    rad_dynrangeW = rad_dynrange / conversion
    radW = np.linspace(0.99*rad_minW, 1.01*(rad_minW+rad_dynrangeW), 1000) 
    lux =  Wm2tolux * radW
    # convert from W back to q/s when setting up the function    
    fintp = interpolate.interp1d((radW*wavelength / (const.h * const.c)).reshape(-1), lux.reshape(-1))
    return fintp


################################################################
################################################################
## 
開發者ID:NelisW,項目名稱:pyradi,代碼行數:42,代碼來源:rytarggen.py


注:本文中的scipy.constants.h方法示例由純淨天空整理自Github/MSDocs等開源代碼及文檔管理平台,相關代碼片段篩選自各路編程大神貢獻的開源項目,源碼版權歸原作者所有,傳播和使用請參考對應項目的License;未經允許,請勿轉載。