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The Origin of Titan’s External Oxygen: Further Constraints from ALMA Upper Limits on CS and CH2NH

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Original languageEnglish
Article number251
Number of pages8
JournalAstronomical Journal
Volume155
Early online date25 May 2018
DOIs
DateAccepted/In press - 27 Apr 2018
DateE-pub ahead of print - 25 May 2018
DatePublished (current) - Jun 2018

Abstract

Titan's atmospheric inventory of oxygen compounds (H2O, CO2, CO) are thought to result from photochemistry acting on externally supplied oxygen species (O+, OH, H2O). These species potentially originate from two main sources: (1) cryogenic plumes from the active moon Enceladus and (2) micrometeoroid ablation. Enceladus is already suspected to be the major O+ source, which is required for CO creation. However, photochemical models also require H2O and OH influx to reproduce observed quantities of CO2 and H2O. Here, we exploit sulphur as a tracer to investigate the oxygen source because it has very different relative abundances in micrometeorites (S/O ~ 10−2) and Enceladus' plumes (S/O ~ 10−5). Photochemical models predict most sulphur is converted to CS in the upper atmosphere, so we use Atacama Large Millimeter/submillimeter Array (ALMA) observations at ~340 GHz to search for CS emission. We determined stringent CS 3σ stratospheric upper limits of 0.0074 ppb (uniform above 100 km) and 0.0256 ppb (uniform above 200 km). These upper limits are not quite stringent enough to distinguish between Enceladus and micrometeorite sources at the 3σ level and a contribution from micrometeorites cannot be ruled out, especially if external flux is toward the lower end of current estimates. Only the high-flux micrometeorite source model of Hickson et al. can be rejected at 3σ. We determined a 3σ stratospheric upper limit for CH2NH of 0.35 ppb, which suggests cosmic rays may have a smaller influence in the lower stratosphere than predicted by some photochemical models. Disk-averaged C3H4 and C2H5CN profiles were determined and are consistent with previous ALMA and Cassini/CIRS measurements.

    Research areas

  • planets and satellites: atmospheres, planets and satellites: individual (Titan), radiative transfer

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    Rights statement: This is the final published version of the article (version of record). It first appeared online via IOP at http://iopscience.iop.org/article/10.3847/1538-3881/aac172 . Please refer to any applicable terms of use of the publisher.

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