The structure of Titan’s atmosphere from Cassini radio occultations

Schinder, P. J.; Flasar, F. M.; Marouf, E. A.; French, R. G.; McGhee, C. A.; Kliore, A. J.; Rappaport, N. J.; Barbinis, E.; Fleischman, D.; Anabtawi, A.

doi:10.1016/j.icarus.2011.07.030

Cited by 52 publications

(56 citation statements)

References 44 publications

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“…That result, 93.65±0.25 K, agrees within the error with our measurements in 2004-2006 (L s = 313°). Between 2005 and 2013 the temperature at the Huygens touchdown latitude had decreased by about 1 K. Our measurements also agree with near-surface temperatures reported by Schinder et al (2011Schinder et al ( , 2012 from Cassini radio occultations. Their 10 reported ingress and egress surface temperatures, near the same latitudes and dates, were on average 0.25 K lower than CIRS with a standard deviation of 0.45 K.…”

Section: Resultssupporting

confidence: 90%

“…The model is based on the temperature profile measured in situ at 0-147 km altitude by the Huygens Atmospheric Structure Instrument (HASI) on the Huygens descent probe (Fulchignoni et al 2005). Modifications were applied to the HASI profile to account for latitude dependences and seasonal variations in temperature found by CIRS and Cassini radio occultations (Coustenis et al 2007(Coustenis et al , 2010(Coustenis et al , 2013(Coustenis et al , 2015Achterberg et al 2008Achterberg et al , 2011Schinder et al 2011Schinder et al , 2012Bampasidis et al 2012). At latitudes greater than about 60°the stratospheric temperature had a minimum in winter near 120 km.…”

Section: Discussionmentioning

confidence: 99%

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Surface Temperatures on Titan During Northern Winter and Spring

Jennings

Cottini

Nixon

et al. 2016

ApJL

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Meridional brightness temperatures were measured on the surface of Titan during the 2004-2014 portion of the Cassini mission by the Composite Infrared Spectrometer. Temperatures mapped from pole to pole during five twoyear periods show a marked seasonal dependence. The surface temperature near the south pole over this time decreased by 2 K from 91.7±0.3 to 89.7±0.5 K while at the north pole the temperature increased by 1 K from 90.7±0.5 to 91.5±0.2 K. The latitude of maximum temperature moved from 19 S to 16 N, tracking the subsolar latitude. As the latitude changed, the maximum temperature remained constant at 93.65±0.15 K. In 2010 our temperatures repeated the north-south symmetry seen by Voyager one Titan year earlier in 1980. Early in the mission, temperatures at all latitudes had agreed with GCM predictions, but by 2014 temperatures in the north were lower than modeled by 1 K. The temperature rise in the north may be delayed by cooling of sea surfaces and moist ground brought on by seasonal methane precipitation and evaporation.

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Section: Resultssupporting

confidence: 90%

Section: Discussionmentioning

confidence: 99%

Surface Temperatures on Titan During Northern Winter and Spring

Jennings

Cottini

Nixon

et al. 2016

ApJL

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“…Table 1 Date, orbit number, encounter number, and latitude and west longitude (in degrees) at the surface for the radio occultations of Cassini by Titan to date. The T12 and T14 profiles were presented in Schinder et al (2011). The soundings T46E, T52I, and T52E will be presented in a later paper.…”

Section: T57mentioning

confidence: 99%

“…1). For comparison, the T14 ingress profile (Schinder et al, 2011) is also shown. et al (2011) have discussed in detail the numerical technique used to determine the structure of the atmosphere and produce temperature-altitude profiles, so we only briefly summarize it here.…”

Section: Datementioning

confidence: 99%

“…During the mission extension known as the Equinox mission, which ended on October 10, 2010, three additional radio occultations occurred during targeted Titan encounters. Schinder et al (2011) reported results obtained from the first two Cassini radio occultations by Titan, T12 and T14 (Tn denotes Titan flyby number n). These all occurred in the southern (summer) hemisphere: three were near 32°S, while the fourth was near 53°S.…”

Section: Introductionmentioning

confidence: 99%

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The structure of Titan’s atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions

Schinder

Flasar

Marouf

et al. 2012

Icarus

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A numerical technique for two‐way radio occultations by oblate axisymmetric atmospheres with zonal winds

et al. 2015

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The Ultra Stable Oscillator aboard the Cassini spacecraft failed in late 2011, which means that all radio occultations after that date have to be done in two‐way mode, using a ground‐based signal transmitted to the spacecraft as the frequency reference. Here we present the numerical technique we use to analyze the data from the two‐way atmospheric radio occultations of both Saturn and Titan that have occurred since the Ultra Stable Oscillator (USO) failure, along with the theoretical reasons behind this technique. Since our two‐way technique is based upon our earlier one‐way technique which used the USO as the frequency reference, we also present our one‐way technique which we used for Saturn occultations prior to the loss of the USO.

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The structure of Titan’s atmosphere from Cassini radio occultations

Cited by 52 publications

References 44 publications

Surface Temperatures on Titan During Northern Winter and Spring

Surface Temperatures on Titan During Northern Winter and Spring

The structure of Titan’s atmosphere from Cassini radio occultations: Occultations from the Prime and Equinox missions

A numerical technique for two‐way radio occultations by oblate axisymmetric atmospheres with zonal winds

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