auricThe Atmospheric Ultraviolet Radiance Integrated Code (AURIC) is a software package originally developed by Computational Physics, Inc. (CPI) for the Air Force Phillips Laboratory (currently the Air Force Research Laboratory [AFRL]) for upper atmospheric radiance modeling from the far ultraviolet to the near infrared. It effectively extends the MODTRAN® code for calculating atmospheric transmittance and radiance (infrared and Rayleigh plus aerosol scattering of sunlight) to earth altitudes above 100 km and wavelengths down to 80 nm.

CPI has made many enhancements to AURIC since its inception, including a more comprehensive chemistry model (for neutral and ionospheric species), new radiative transfer capabilities, the option of performing photoelectron energy degradation with or without transport, updates to electron impact cross sections and the addition of new emission features. AURIC is currently in use by a number of organizations: The Naval Research Laboratory, Johns Hopkins Applied Physics Laboratory, Laboratory for Atmospheric and Space Physics (University of Colorado), Southwest Research Institute, and the Slovak Academy of Sciences.  The most recent applications of AURIC have been for the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission and the New Horizons encounter with the Pluto – Charon system.  A summary of AURIC's modeling capabilities can be found in the AURIC brochure. Examples of applications papers using AURIC are listed in the references below.

AURIC has been validated against numerous published rocket and satellite data, and shown to have good overall agreement with the measurements. The airglow modeling capabilities of AURIC make it a powerful tool for characterizing optical backgrounds at thermospheric altitudes, for developing remote sensing algorithms, for simulating data from rocket and satellite optical instrumentation, and for conducting science investigations (both sensitivity studies and data analyses)..

OII 834 Å 3D Simulation





AURIC 3D Simulation using IDA4D

AURIC consists of portable Fortran source code for calculating airglow spectral radiances and densities of chemically active species. Both text-based and command-line user interfaces are provided for tailoring the execution of the model for specific applications. In line with its operational status, the software compiles and executes under both Linux and Mac operating systems.   An AURIC Users Manual has also been written with detailed information for operating the model on Linux and Mac OS platforms, along with numerous tables and illustrations of inputs and outputs. To learn more about AURIC, please contact us.

AURIC limb profiles

Limb profiles in Rayleighs for 60° solar zenith .angle and a Hinteregger solar EUV spectrum based on F10.7 = 150, plus profiles for the optically thick OI 1304 Å and HI 1216 Å features. The difference in shape between the two LBH profiles is due to differences in O2 Schumann-Runge opacity.


Siskind, David E.; Strickland, D. J.; Meier, R. R.; Majeed, T.; Eparvier, F. G. (1995), On the Relationship Between the Solar Soft X Ray Flux and Thermospheric Nitric Oxide: An Update with an Improved Photoelectron Model, J. Geophys. Res., 100(A10), 19687–19694, doi:10.1029/95JA01609.

Strickland, D. J.; Evans, J. S.; Paxton, L. J (1995), Satellite Remote Sensing of Thermospheric O/N2 and solar EUV, 1. Theory, J. Geophys. Res., 10(A7), 12217–12226, doi:10.1029/95JA00574.

Majeed, T.; and Strickland, D. J. (1997), New Survey of Electron Impact Cross Sections for Photoelectron and Auroral Electron Energy Loss Calculations, J. Phys. Chem. Ref. Data, 26(2), 335, doi:10.1063/1.556008.

Strickland, D. J.; Majeed, T.; Evans, J. S.; Meier, R. R.; Picone, J. M. (1997), Analytical representation of g factors for rapid, accurate calculation of excitation rates in the dayside thermosphere, J. Geophys. Res., 102(A7), 14485–14498, doi:10.1029/97JA00943.

Strickland, D. J., J. Bishop, J.S. Evans, T. Majeed, P.M. Shen, R.J. Cox, R. Link, R.E. Huffman (1999), Atmospheric Ultraviolet Radiance Integrated Code (AURIC): theory, software architecture, inputs, and selected results, Journal of Quantitative Spectroscopy & Radiative Transfer, 62(6), 689-742, doi:10.1016/S0022-4073(98)00098-3.

Bishop, J., M.H. Stevens and P.D. Feldman (2007), Molecular nitrogen Carroll-Yoshino v’=0 emission in the thermospheric dayglow as seen by the Far Ultraviolet Spectroscopic Explorer (2007), J. Geophys. Res., 112, A10312, doi:10.1029/2007/JA012389.

Stevens, M. H., J. S. Evans, J. D. Lumpe, J. H. Westlake, J. M. Ajello, E. T. Bradley, and L. W. Esposito (2015), Molecular nitrogen and methane density retrievals from Cassini UVIS dayglow observations of Titan’s upper atmosphere, Icarus 247, 301–312.

Evans, J.S., et al. (2015), Retrieval of CO2 and N2 in the Martian Thermosphere using dayglow observations by IUVS on MAVEN, Geophys. Res. Lett., 42, doi:10.1002/2015GL065489

Stevens, M. H., et al. (2015), New observations of molecular nitrogen in the Martian upper atmosphere by IUVS on MAVEN, Geophys. Res. Lett., 42, 9050–9056, doi:10.1002/2015GL065319.

Schindelm, E., S.A. Stern, R. Gladstone and A. Zangari (2015), Pluto and Charon’s UV spectra from IUE to New Horizons, Icarus, 246, 206-212.

Schneider, N. M., et al. (2015), Discovery of diffuse aurora on Mars, Science, vol. 350, no. 6261; doi: 10.1126/science.aad0313.