<reponame>saultyevil/PyPython<filename>pypython/physics/blackbody.py
#!/usr/bin/env python3
# -*- coding: utf-8 -*-
"""Blackbody functions for wavelength and frequency.

In wavelength space, the blackbody function assumes that the wavelength
is given in units of Angstroms.
"""

import numpy as np
from numba import jit

from pypython.constants import (ANGSTROM, BOLTZMANN, VLIGHT, WIEN_FREQUENCY, WIEN_WAVELENGTH, H, PI, STEFAN_BOLTZMANN)


@jit
def planck_lambda(temperature, lamda):
    """Calculate the monochromatic intensity for a black body given a
    temperature and frequency of interest.

    Parameters
    ----------
    temperature: float
        The temperature of the blackbody.
    lamda: np.ndarray or float
        The wavelength points to calculate the value at, in Angstroms.

    Returns
    -------
    b_lamda: float
        The value of the Planck function with the provided temperature and
        wavelength. Has units ergs s^-1 cm^-2 A^-1.
    """

    lcm = lamda * ANGSTROM
    x = H * VLIGHT / lcm / BOLTZMANN / temperature
    y = 2 * H * VLIGHT**2 / lcm**5
    b_lamda = y / (np.exp(x) - 1)

    return b_lamda


@jit
def planck_nu(temperature, frequency):
    """Calculate the monochromatic intensity for a black body given a
    temperature and frequency of interest.

    Parameters
    ----------
    temperature: float
        The temperature of the blackbody.
    frequency: np.ndarray or float
        The frequency points to calculate the vale at, in units of Hz.

    Returns
    -------
    b_nu: float
        The value of the Planck function with the provided temperature and
        frequency. Has units ergs s^-1 cm^-2 Hz^-1.
    """

    x = H * frequency / (BOLTZMANN * temperature)
    b_nu = (2 * H * frequency**3) / (VLIGHT**2 * (np.exp(x) - 1))

    return b_nu


def stefan_boltzmann(radius, temperature):
    """Calculate the luminosity for a spherical blackbody following from
    Stefan-Boltzmann.

    Parameters
    ----------
    radius: float
        The radius of the sphere.
    temperature: float
        The temperature of the blackbody.

    Returns
    -------
    lum: float
        The luminosity of the sphere.
    """
    return 4 * PI * radius**2 * STEFAN_BOLTZMANN * temperature**4


def wien_law(temperature, freq_space=False):
    """Calculate the peak wavelength of a blackbody curve.

    Parameters
    ----------
    temperature: float
        The temperature of the blackbody.
    freq_space: bool [optional]
        Return the peak in frequency space.

    Returns
    -------
    The wavelength (in Angstrom) or frequency where the blackbody curve is
    at maximum.
    """

    if freq_space:
        return WIEN_FREQUENCY * temperature
    else:
        return WIEN_WAVELENGTH / temperature / 1e-10

#!/usr/bin/env python3
# -*- coding: utf-8 -*-
"""Blackbody functions for wavelength and frequency.

In wavelength space, the blackbody function assumes that the wavelength
is given in units of Angstroms.
"""

import numpy as np
from numba import jit

from pypython.constants import (ANGSTROM, BOLTZMANN, VLIGHT, WIEN_FREQUENCY, WIEN_WAVELENGTH, H, PI, STEFAN_BOLTZMANN)


@jit
def planck_lambda(temperature, lamda):
    """Calculate the monochromatic intensity for a black body given a
    temperature and frequency of interest.

    Parameters
    ----------
    temperature: float
        The temperature of the blackbody.
    lamda: np.ndarray or float
        The wavelength points to calculate the value at, in Angstroms.

    Returns
    -------
    b_lamda: float
        The value of the Planck function with the provided temperature and
        wavelength. Has units ergs s^-1 cm^-2 A^-1.
    """

    lcm = lamda * ANGSTROM
    x = H * VLIGHT / lcm / BOLTZMANN / temperature
    y = 2 * H * VLIGHT**2 / lcm**5
    b_lamda = y / (np.exp(x) - 1)

    return b_lamda


@jit
def planck_nu(temperature, frequency):
    """Calculate the monochromatic intensity for a black body given a
    temperature and frequency of interest.

    Parameters
    ----------
    temperature: float
        The temperature of the blackbody.
    frequency: np.ndarray or float
        The frequency points to calculate the vale at, in units of Hz.

    Returns
    -------
    b_nu: float
        The value of the Planck function with the provided temperature and
        frequency. Has units ergs s^-1 cm^-2 Hz^-1.
    """

    x = H * frequency / (BOLTZMANN * temperature)
    b_nu = (2 * H * frequency**3) / (VLIGHT**2 * (np.exp(x) - 1))

    return b_nu


def stefan_boltzmann(radius, temperature):
    """Calculate the luminosity for a spherical blackbody following from
    Stefan-Boltzmann.

    Parameters
    ----------
    radius: float
        The radius of the sphere.
    temperature: float
        The temperature of the blackbody.

    Returns
    -------
    lum: float
        The luminosity of the sphere.
    """
    return 4 * PI * radius**2 * STEFAN_BOLTZMANN * temperature**4


def wien_law(temperature, freq_space=False):
    """Calculate the peak wavelength of a blackbody curve.

    Parameters
    ----------
    temperature: float
        The temperature of the blackbody.
    freq_space: bool [optional]
        Return the peak in frequency space.

    Returns
    -------
    The wavelength (in Angstrom) or frequency where the blackbody curve is
    at maximum.
    """

    if freq_space:
        return WIEN_FREQUENCY * temperature
    else:
        return WIEN_WAVELENGTH / temperature / 1e-10
#!/usr/bin/env python3 # -*- coding: utf-8 -*- Blackbody functions for wavelength and frequency.  In wavelength space, the blackbody function assumes that the wavelength is given in units of Angstroms. Calculate the monochromatic intensity for a black body given a     temperature and frequency of interest.      Parameters     ----------     temperature: float         The temperature of the blackbody.     lamda: np.ndarray or float         The wavelength points to calculate the value at, in Angstroms.      Returns     -------     b_lamda: float         The value of the Planck function with the provided temperature and         wavelength. Has units ergs s^-1 cm^-2 A^-1. Calculate the monochromatic intensity for a black body given a     temperature and frequency of interest.      Parameters     ----------     temperature: float         The temperature of the blackbody.     frequency: np.ndarray or float         The frequency points to calculate the vale at, in units of Hz.      Returns     -------     b_nu: float         The value of the Planck function with the provided temperature and         frequency. Has units ergs s^-1 cm^-2 Hz^-1. Calculate the luminosity for a spherical blackbody following from     Stefan-Boltzmann.      Parameters     ----------     radius: float         The radius of the sphere.     temperature: float         The temperature of the blackbody.      Returns     -------     lum: float         The luminosity of the sphere. Calculate the peak wavelength of a blackbody curve.      Parameters     ----------     temperature: float         The temperature of the blackbody.     freq_space: bool [optional]         Return the peak in frequency space.      Returns     -------     The wavelength (in Angstrom) or frequency where the blackbody curve is     at maximum.