Titan's Nitrogen Emissions: Spatial, Temporal, and Hemispherical Distribution and Variability as Measured by Cassini-UVIS.

Details Titan's Nitrogen Emissions: Spatial, Temporal, and Hemispherical Distribution and Variability as Measured by Cassini-UVIS. Titan's Nitrogen Emissions: Spatial, Temporal, and Hemispherical Distribution and Variability as Measured by Cassini-UVIS.

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p23b1363l&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #P23B-1363

Physics

5405 Atmospheres (0343, 1060), 5408 Aurorae And Airglow, 6281 Titan

Scientific paper

As of September 1, 2007, the Cassini spacecraft has conducted 35 fly-by's of Titan in which the UltraViolet Imaging Spectrograph (UVIS) conducted observations. Used in this investigation is a sub-set of Titan observations, twenty-three in total, that viewed the entirety of Titan's dayside, nightside, or some combination of both bracketing the terminator, with the high resolution Far UltraViolet (FUV) channel (1120 - 1910 Å). Unlike observations during the Voyager missions, this extended monitoring period has provided greater insight into the distribution and temporal variability of emissions from Titan, in particular those of the nitrogen Lyman- Birge-Hopfield (LBH) bands. Not only does the UVIS instrument provide finer spatial and spectral resolution, but the observations spread over the first three years of the mission have provided the opportunity to examine the role of Saturn's magnetosphere on the distribution and intensity of Titan's nitrogen emissions as Titan has been observed at a variety of locations within the magnetosphere. Titan's nitrogen emissions have shown wide variability during Cassini's primary mission, in particular those emissions emanating from the nightside disk. Emissions from the nitrogen LBH bands are uniformly present on Titan's dayside disk with maximum intensities of approximately 0.5 Rayleighs/Å*pixel in the strongest of the LBH bands. Nitrogen LBH emissions, from observations that imaged both day and nightside disks, range from 0 to 50% the intensity of the dayside emissions. The variability of the nightside emissions appears uncorrelated with Titan's location within Saturn's magnetosphere. The high spatial resolution of the UVIS instrument has been used to probe the vertical and spatial variability of the nitrogen LBH emissions on both the day and nightside of Titan. Nitrogen emissions from Tita's dayside, both from the LBH and atomic N-I and N-II bands, peak at an altitude of 1100±50 km above the surface of Titan, while emissions from the nightside show a peak altitude of 1000±50 km.

Affiliated with

Also associated with

No associations

Rating

Titan's Nitrogen Emissions: Spatial, Temporal, and Hemispherical Distribution and Variability as Measured by Cassini-UVIS. does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Titan's Nitrogen Emissions: Spatial, Temporal, and Hemispherical Distribution and Variability as Measured by Cassini-UVIS., we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Titan's Nitrogen Emissions: Spatial, Temporal, and Hemispherical Distribution and Variability as Measured by Cassini-UVIS. will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1405953