1. J. AJELLO I. STEWART M. STEVENS A.AGUILAR K. LARSEN
COMPARISON OF TITAN EUV AIRGLOW SPECTRA WITH FUSE EARTH AND LABORATORY SPECTRA
J. AJELLO
I. STEWART
M. STEVENS
A.AGUILAR
K. LARSEN

2. UVIS GOALS OVERPLOT SPECTRA (UVIS,FUSE, LAB) LAB GOALS:
IDENTIFICATION OF EUV UVIS FEATURES FROM HIGH RESOLUTION LAB SPECTRA (0.05 TO 0.6 A FWHM)
APPROXIMATE PHOTOELECTRON EXCITATION-MEAN ENERGY BY COMPARING eV LAB SPECTRA
NITROGEN FOREGROUND ABUNDANCES
MEASURE Qem AND hpre.FOR MODELS
LONG RANGE GOALS-COMPARE SPACE WEATHER (THERMAL STRUCTURE, COMPOSITION AND SOLAR ENERGY INPUT) OF EARTH FROM FUSE AND OF TITAN FROM UVIS SPECTRA
INCLUDE SOLAR PHOTIONIZATION AND e + N

3. LABORATORY COMPARISON TO TITAN EUV SPECTRUM

4. COMPARISON OF TITAN, FUSE AND LABORATORY (OPTICALLY THICK h=1015 cm-2) EUV SPECTRA

5. COMPARE SPECTRA AT UVIS 4A FWHM NORMALIZED TO N2 c’(3,2;4,3) AT 943 A

6. IDENITIFICATION OF OVER 100 FEATURES FROM N AND N2 OVER RANGE OF 850-1150 A

13. CONCLUSIONS
EARTH AND TITAN PRESENT SIMILAR EUV SPECTRA
OVER 100 N AND N2 FEATURES CONTRIBUTE TO TITAN EUV CHANNEL UVIS SPECTRA
EXCEPT FOR N2(c’[0,1]) BAND UVIS SPECTRUM IS WELL-MATCHED BY eV OPTICALLY THICK LAB SPECTRA OF e + N2