%0 Journal Article %1 m2007titan %A Ajello, Joseph M. %A Stevens, Michael H. %A Stewart, Ian %A Larsen, Kristopher %A Esposito, Larry %A Colwell, Josh %A McClintock, William %A Holsclaw, Greg %A Gustin, Jacques %A Pryor, Wayne %D 2007 %I AGU %J Geophys. Res. Lett. %K airglow cassini spectra titan ultraviolet %N 24 %P L24204-- %T Titan airglow spectra from Cassini Ultraviolet Imaging Spectrograph (UVIS): EUV analysis %U http://dx.doi.org/10.1029/2007GL031555 %V 34 %X We present the first UV airglow observations of Titan's atmosphere by the Ultraviolet Imaging Spectrograph (UVIS) on Cassini. Using one spectral channel in the EUV from 561–1182 � and one in the FUV from 1115–1913 �, UVIS observed the disk on 13 December, 2004 at low solar activity. The EUV spectrum consists of three band systems of N2 (b 1∏u, b′ 1∑u +, c4′ 1∑u + → X 1∑g +), while the FUV spectrum consists of one (a 1∏g → X 1∑g +). Both the EUV and FUV spectra contain many N I and N II multiplets that are produced primarily by photodissociative ionization. Spectral intensities of the N2 c4′ 1∑u +(v′ = 0) → X 1∑g +(v″ = 0–2) progression from 950–1010 � are resolved for the first time. The UVIS observations reveal that the c4′ 1∑u +(0) → X 1∑g + (0) vibrational band near 958 � is weak and undetectable, and that N I multiplets near 953.2 and 964.5 � are present instead. Magnetospheric particle excitation may be weak or sporadic, since the nightside EUV spectrum on this orbit shows no observable nitrogen emission features and only H Ly-β.

@article{m2007titan, abstract = {We present the first UV airglow observations of Titan's atmosphere by the Ultraviolet Imaging Spectrograph (UVIS) on Cassini. Using one spectral channel in the EUV from 561–1182 � and one in the FUV from 1115–1913 �, UVIS observed the disk on 13 December, 2004 at low solar activity. The EUV spectrum consists of three band systems of N2 (b 1∏u, b′ 1∑u +, c4′ 1∑u + → X 1∑g +), while the FUV spectrum consists of one (a 1∏g → X 1∑g +). Both the EUV and FUV spectra contain many N I and N II multiplets that are produced primarily by photodissociative ionization. Spectral intensities of the N2 c4′ 1∑u +(v′ = 0) → X 1∑g +(v″ = 0–2) progression from 950–1010 � are resolved for the first time. The UVIS observations reveal that the c4′ 1∑u +(0) → X 1∑g + (0) vibrational band near 958 � is weak and undetectable, and that N I multiplets near 953.2 and 964.5 � are present instead. Magnetospheric particle excitation may be weak or sporadic, since the nightside EUV spectrum on this orbit shows no observable nitrogen emission features and only H Ly-β.}, added-at = {2010-05-16T12:56:54.000+0200}, author = {Ajello, Joseph M. and Stevens, Michael H. and Stewart, Ian and Larsen, Kristopher and Esposito, Larry and Colwell, Josh and McClintock, William and Holsclaw, Greg and Gustin, Jacques and Pryor, Wayne}, biburl = {https://www.bibsonomy.org/bibtex/2f6a94cd0ca9e9f9b846442d1b3fa24a3/gensemer}, description = {Titan airglow spectra from Cassini Ultraviolet Imaging Spectrograph (UVIS): EUV analysis}, interhash = {53b76cd95bc8d08fe428cdfc75f18175}, intrahash = {f6a94cd0ca9e9f9b846442d1b3fa24a3}, issn = {00948276}, journal = {Geophys. Res. Lett.}, keywords = {airglow cassini spectra titan ultraviolet}, month = {#dec#}, number = 24, pages = {L24204--}, publisher = {AGU}, timestamp = {2010-05-16T12:56:54.000+0200}, title = {Titan airglow spectra from Cassini Ultraviolet Imaging Spectrograph (UVIS): EUV analysis}, url = {http://dx.doi.org/10.1029/2007GL031555}, volume = 34, year = 2007 }