eppaurora 0.2.0

Atomspheric ionization from auroral particle precipitation

PyEPPAurora

Atmospheric ionization from particle precipitation

Bundles some of the parametrizations for middle and upper atmospheric ionization and recombination rates for precipitating auroral and radiation-belt electrons as well as protons. Includes also some recombination rate parametrizations to convert the ionization rates to electron densities in the upper atmosphere. See References for a list of included parametrizations.

:warning: This package is in beta stage, that is, it works for the most part and the interface should not change (much) in future versions.

Documentation is available at https://pyeppaurora.readthedocs.io.

Install

Requirements

• numpy - required
• scipy - required for 2-D interpolation
• pytest - optional, for testing

eppaurora

An installable pip package called eppaurora is available from the main package repository, it can be installed with:

$ pip install eppaurora

The latest development version can be installed with pip directly from github (see https://pip.pypa.io/en/stable/reference/pip_install/#vcs-support and https://pip.pypa.io/en/stable/reference/pip_install/#git):

$ pip install [-e] git+https://github.com/st-bender/pyeppaurora.git

The other option is to use a local clone:

$ git clone https://github.com/st-bender/pyeppaurora.git
$ cd pyeppaurora

and then using pip (optionally using -e, see https://pip.pypa.io/en/stable/reference/pip_install/#install-editable):

$ pip install [-e] .

or using setup.py:

$ python setup.py install

Optionally, test the correct function of the module with

$ py.test [-v]

or even including the doctests in this document:

$ py.test [-v] --doctest-glob='*.md'

Usage

The python module itself is named eppaurora and is imported as usual.

All functions should be numpy-compatible and work with scalars and appropriately shaped arrays.

>>> import eppaurora as aur
>>> ediss = aur.rr1987(1., 1., 8e5, 5e-10)
>>> ediss
3.3693621076457477e-10
>>> import numpy as np
>>> energies = np.logspace(-1, 2, 4)
>>> fluxes = np.ones_like(energies)
>>> # ca. 100, 150, 200 km
>>> scale_heights = np.array([6e5, 27e5, 40e5])
>>> rhos = np.array([5e-10, 1.7e-12, 2.6e-13])
>>> # energy dissipation "profiles"
>>> # broadcast to the right shape
>>> ediss_prof = aur.fang2008(
... 	energies[None, :], fluxes[None, :],
... 	scale_heights[:, None], rhos[:, None]
... )
>>> ediss_prof
array([[1.37708081e-49, 3.04153876e-09, 4.44256875e-07, 2.52699970e-08],
       [1.60060833e-09, 8.63248169e-08, 3.64564419e-09, 1.62591310e-10],
       [5.19369952e-08, 2.34089350e-08, 5.17379303e-10, 3.19504690e-11]])

Basic class and method documentation is accessible via pydoc:

$ pydoc eppaurora
$ pydoc eppaurora.brems
$ pydoc eppaurora.conductivity
$ pydoc eppaurora.electrons
$ pydoc eppaurora.protons
$ pydoc eppaurora.recombination

References

Electron ionization

[1]: Roble and Ridley, Ann. Geophys., 5A(6), 369--382, 1987
[2]: Fang et al., J. Geophys. Res. Space Phys., 113, A09311, 2008, doi: 10.1029/2008JA013384
[3]: Fang et al., Geophys. Res. Lett., 37, L22106, 2010, doi: 10.1029/2010GL045406

Ionization by secondary electrons from bremsstrahlung

[4]: Berger et al., Journal of Atmospheric and Terrestrial Physics, Volume 36, Issue 4, 591--617, April 1974, doi: 10.1016/0021-9169(74)90085-3

Proton ionization

[5]: Fang et al., J. Geophys. Res. Space Phys., 118, 5369--5378, 2013, doi: 10.1002/jgra.50484

Recombination rates

[6]: Vickrey et al., J. Geophys. Res. Space Phys., 87, A7, 5184--5196, doi: 10.1029/ja087ia07p05184
[7]: Gledhill, Radio Sci., 21, 3, 399-408, doi: 10.1029/rs021i003p00399
[8]: https://ssusi.jhuapl.edu/data_algorithms

Conductivity and conductance

[9]: Brekke et al., J. Geophys. Res., 79(25), 3773--3790, Sept. 1974, doi: 10.1029/JA079i025p03773
[10]: Vickrey et al., J. Geophys. Res., 86(A1), 65--75, Jan. 1981, doi: 10.1029/JA086iA01p00065
[11]: Robinson et al., J. Geophys. Res. Space Phys., 92(A3), 2565--2569, Mar. 1987, doi: 10.1029/JA092iA03p02565

License

This python interface is free software: you can redistribute it or modify it under the terms of the GNU General Public License as published by the Free Software Foundation, version 2 (GPLv2), see local copy or online version.