Ideas for Further Study Proton impact excitation in the region 300-1000 km
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Airglow on Titan During Eclipse R. A. West 1 , J. M. Ajello 1 , M. H. Stevens 2 , D. F. Strobel 3 , G. R. Gladstone 4 , J.S. Evans 5 , E.T. Bradley 6 1 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 USA, 2 US Naval, Res Lab, Div Space Sci, Washington, DC 20375 USA, 3 Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA, 4 SW Res Inst, Space Sci & Engn Div, San Antonio, TX 78238 USA, 5 Comp. Phys. Inc, Springfield, VA 22151 USA, 6 Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA ([email protected]) Titan dayglow spectra observed by Cassini UVIS (from Stevens et al., JGR Space Physics 116, 2011) for reference. Ideas for Further Study • Proton impact excitation in the region 300-1000 km • Cosmic Ray ionization deeper than 300 km • Chemiluminescence and flow onto the nightside (possibly CN emission) Eclipse EUV Spectrum Eclipse FUV Spectrum. Fits to lines and bands are shown in lower panels. Illuminated by sunlight from Saturn’s limb. Max I/F = 4X10 -6 Bottom Panel: Scattered sunlight component was subtracted; Max I/F = 2X10-7 Deep airglow from within Titan’s haze (below 300 km altitude). Very faint glow between 300 and 1000 km. This work from West et al., Geophys. Res. Lett . 39, L18204, doi:10.1029/2012GL053230, 2012
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Airglow on Titan During Eclipse
R. A. West1, J. M. Ajello1, M. H. Stevens2, D. F. Strobel3, G. R. Gladstone4, J.S. Evans5, E.T. Bradley6
1 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109 USA, 2 US Naval, Res Lab, Div Space Sci, Washington, DC 20375 USA, 3Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA, 4SW Res Inst, Space
Sci & Engn Div, San Antonio, TX 78238 USA, 5Comp. Phys. Inc, Springfield, VA 22151 USA, 6Univ Cent Florida, Dept Phys, Orlando, FL 32816 USA
Titan dayglow spectra observed by Cassini UVIS (from Stevens et al., JGR Space Physics 116, 2011) for reference.
Ideas for Further Study
•Proton impact excitation in the region 300-1000 km
•Cosmic Ray ionization deeper than 300 km
•Chemiluminescence and flow onto the nightside (possibly CN emission)
Eclipse EUV Spectrum
Eclipse FUV Spectrum.Fits to lines and bandsare shown in lower panels.
Illuminated by sunlight from Saturn’s limb. Max I/F = 4X10-6
Bottom Panel: Scattered sunlightcomponent was subtracted; Max I/F = 2X10-7
Deep airglow from within Titan’s haze (below 300 km altitude).
Very faint glow between 300 and 1000 km.
This work from West et al., Geophys. Res. Lett. 39, L18204, doi:10.1029/2012GL053230, 2012
