PDS: The Planetary Atmospheres Node
Location of the Cassini UV and IR Spectrographs
Introduction
The data were derived by combining measurements from stellar occultations observed by the extreme ultraviolet component (EUV) of the Cassini Ultraviolet Imaging Spectrograph (UVIS) and limb scans observed by the Composite Infrared Spectrometer (CIRS) to create empirical atmospheric structure models for Saturn corresponding to the locations probed by the occultations. Temperature-pressure (T-P) profiles retrieved from the CIRS limb scans in the stratosphere were combined with T-P profiles in the thermosphere retrieved from the UVIS occultations. Altitudes corresponding to the pressure levels in each case were derived based on a best fit composition model that included H2, He, CH4 and upper limits on H.
References
Koskinen T.T., Sandel B.R., Yelle R.V., Strobel D.F., Muller-Wodarg I.C.F, Erwin J.T., 2015., Saturn's variable thermosphere from Cassini/UVIS occultations. Icarus 260, 174-189, DOI 10.1016/j.icarus.2015.07.008.
Koskinen T.T., Moses J.I., West R.A., Guerlet S., Jouchoux A., 2015., The detection of benzene in Saturn’s upper atmosphere. GRL 43 7895-7901, DOI 10.1002/2016GL070000.
Koskinen T.T., Guerlet S., 2018. Atmospheric structure and helium abundance on Saturn from Cassini/UVIS and CIRS observations., Icarus 307 161-171, DOI 10.1016/j.icarus.2018.02.020.
Description of the Data
Documentation
The results cover a range of low to mid-latitudes between the spring of 2005 and the fall of 2015. The tables contain values for Altitude, Radius, Latitude, Longitude, H2 Number Density, Temperature and Number Density and Temperature from a forward model (Koskinen T.T., Sandel B.R., et al. 2015).
Accessing the data
Each data file is specified by a unique identifier (URN). An index (CSV) is provided to aid in product selection. Some values in the table may not be consistent.
Downloading the data Will be linked to a compressed file of the bundle
Citing the data
Koskinen (2020), Saturn Thermosphere, NASA Planetary Data System, doi:
The data were derived by combining measurements from stellar occultations observed by the extreme ultraviolet component (EUV) of the Cassini Ultraviolet Imaging Spectrograph (UVIS) and limb scans observed by the Composite Infrared Spectrometer (CIRS) to create empirical atmospheric structure models for Saturn corresponding to the locations probed by the occultations. Temperature-pressure (T-P) profiles retrieved from the CIRS limb scans in the stratosphere were combined with T-P profiles in the thermosphere retrieved from the UVIS occultations. Altitudes corresponding to the pressure levels in each case were derived based on a best fit composition model that included H2, He, CH4 and upper limits on H.
References
Koskinen T.T., Sandel B.R., Yelle R.V., Strobel D.F., Muller-Wodarg I.C.F, Erwin J.T., 2015., Saturn's variable thermosphere from Cassini/UVIS occultations. Icarus 260, 174-189, DOI 10.1016/j.icarus.2015.07.008.
Koskinen T.T., Moses J.I., West R.A., Guerlet S., Jouchoux A., 2015., The detection of benzene in Saturn’s upper atmosphere. GRL 43 7895-7901, DOI 10.1002/2016GL070000.
Koskinen T.T., Guerlet S., 2018. Atmospheric structure and helium abundance on Saturn from Cassini/UVIS and CIRS observations., Icarus 307 161-171, DOI 10.1016/j.icarus.2018.02.020.
Description of the Data
Documentation
The results cover a range of low to mid-latitudes between the spring of 2005 and the fall of 2015. The tables contain values for Altitude, Radius, Latitude, Longitude, H2 Number Density, Temperature and Number Density and Temperature from a forward model (Koskinen T.T., Sandel B.R., et al. 2015).
Accessing the data
Each data file is specified by a unique identifier (URN). An index (CSV) is provided to aid in product selection. Some values in the table may not be consistent.
Downloading the data Will be linked to a compressed file of the bundle
Citing the data
Koskinen (2020), Saturn Thermosphere, NASA Planetary Data System, doi:
