J. AJELLO I. STEWART M. STEVENS A.AGUILAR K. LARSEN

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Presentation transcript:

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

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 20-100 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

LABORATORY COMPARISON TO TITAN EUV SPECTRUM

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

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

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

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 20-30 eV OPTICALLY THICK LAB SPECTRA OF e + N2