Simulated GOLD Observations of Atmospheric Waves

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Presentation transcript:

Simulated GOLD Observations of Atmospheric Waves John Correira1, J. Scott Evans1, Jerry D. Lumpe1, Mihail Codrescu2, David W. Rusch3, Amal Chandran3, Richard Eastes4, and the GOLD Science Team Computational Physics, Inc. NOAA Space Weather Prediction Center Laboratory for Atmospheric and Space Physics, University of Colorado Florida Space Institute, University of Central Florida Acknowledge Dave & Amal for helping get early version of this effort started. Thank Mihail for providing CTIPe model results. Ended up being more about ‘Simulated GOLD observations’ than ‘Atmospheric Waves’

Overview GOLD Day Disk Data Simulations L1C Data Model O/N2 Level 2 Derived O/N2

GOLD Disk Measurement Schedule Spacecraft Local Time Day Disk 24 minutes/scan Occultation Limb 24 minutes per scan + 6 minutes for Occ or Limb = 30 minute cadence

L1C into data processing pipeline Simulations Solar spectra NRLEUV scaled by SEE Atmosphere CTIPe Ionosphere IRI AURIC upper atmospheric radiance modeling from the FUV to the NIR [Strickland et al., 1999] Also used for testing Level 2 pipeline and algorithm codes GNU parallel allowed work to be distributed over 100 cores L1C & L2 data will be NetCDF Geolocation SPICE AURIC volume emission rates Simulated L1C files L1C into data processing pipeline LOSI_3D database atomic emissions Simulated L2 files LOS integration AURIC N2 LBH model Time varying solar spectra, can and will simulate flares Note that LOSI_3D handles the atomic emissions

O/N2 Algorithm Ratio of column density of O above the altitude where the N2 column density is 1017 cm-2 Intensity ratio & SZA uniquely specifies O/N2 Inputs: 1356/LBH intensity ratio, uncertainties, SZA, look up table Signature of atmospheric dynamics GOLD spectral resolution allows for flexibility in choosing best LBH bands Strickland, Evans, and Paxton, JGR, 100, A7, 1995

Model O/N2 CTIPe results for 25 Oct 2015 DOY 298 10 minute cadence Could use to implement time variation of atmosphere during course of single scan 18° longitude spacing 2° latitude spacing Altitude range 75 km ~ 415 km

Example L1C data DOY 298, UT 1500, LT 1200 125 km x 125 km @ nadir Hemispheres scanned separately Slit will overlap 1 degree at equator Both hemispheres included in L1C & L2 files Combined here LBH roughly equivalent to GUVI LBH ‘Short’ (141 - 154 nm) Note disk scan starts two steps off disk. Two hemispheres not temporally coincident in real data. Auroral emssions not included at this stage, will be included in the future (algorithms required an auroral contamination flag) This is not pixelation of the image, this is the L1C grid

Level 2 O/N2 data 250 km x 250 km @ nadir 2x2 binning of Level 1C data Constraints SZA < 80° Emission Angle < 75° Currently emission angle effects are not included in look up tables.

Summary Simulations will help demonstrate the feasibility of detecting various atmospheric phenomena. Multi purpose Test algorithms Observation strategies Provide realistic data processing pipeline codes Future work Incorporate instrument Auroral emissions Solar flares Simulated O/N2 suggest interesting features will be observable

Extra Slides

1356 disk only

1356 with limb

LBH disk only

LBH with limb

1356/LBH Intensity Ratio