Detection of CH3C3N in Titan's atmosphere
Titan harbors a dense, organic-rich atmosphere primarily composed of N2 and CH4, with lesser amounts of hydrocarbons and nitrogen-bearing species. As a result of high-sensitivity observations by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6 (∼230–272 GHz), we obtained the first s...
| Main Authors: | , , , , , , , , |
|---|---|
| Format: | Journal article |
| Language: | English |
| Published: |
IOP Publishing
2020
|
| _version_ | 1826295629075185664 |
|---|---|
| author | Thelen, AE Cordiner, MA Nixon, CA Vuitton, V Kisiel, Z Charnley, SB Palmer, MY Teanby, NA Irwin, PGJ |
| author_facet | Thelen, AE Cordiner, MA Nixon, CA Vuitton, V Kisiel, Z Charnley, SB Palmer, MY Teanby, NA Irwin, PGJ |
| author_sort | Thelen, AE |
| collection | OXFORD |
| description | Titan harbors a dense, organic-rich atmosphere primarily composed of N2 and CH4, with lesser amounts of hydrocarbons and nitrogen-bearing species. As a result of high-sensitivity observations by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6 (∼230–272 GHz), we obtained the first spectroscopic detection of CH3C3N (methylcyanoacetylene or cyanopropyne) in Titan's atmosphere through the observation of seven transitions in the $J=64\to 63$ and $J=62\to 61$ rotational bands. The presence of CH3C3N on Titan was suggested by the Cassini Ion and Neutral Mass Spectrometer detection of its protonated form: C4H3NH+, but the atmospheric abundance of the associated (deprotonated) neutral product is not well constrained due to the lack of appropriate laboratory reaction data. Here, we derive the column density of CH3C3N to be (3.8–5.7) × 1012 cm−2 based on radiative transfer models sensitive to altitudes above 400 km Titan's middle atmosphere. When compared with laboratory and photochemical model results, the detection of methylcyanoacetylene provides important constraints for the determination of the associated production pathways (such as those involving CN, CCN, and hydrocarbons), and reaction rate coefficients. These results also further demonstrate the importance of ALMA and (sub)millimeter spectroscopy for future investigations of Titan's organic inventory and atmospheric chemistry, as CH3C3N marks the heaviest polar molecule detected spectroscopically in Titan's atmosphere to date. |
| first_indexed | 2024-03-07T04:03:59Z |
| format | Journal article |
| id | oxford-uuid:c5866739-723a-4354-94f4-043ea783f49f |
| institution | University of Oxford |
| language | English |
| last_indexed | 2024-03-07T04:03:59Z |
| publishDate | 2020 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | oxford-uuid:c5866739-723a-4354-94f4-043ea783f49f2022-03-27T06:31:38ZDetection of CH3C3N in Titan's atmosphereJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:c5866739-723a-4354-94f4-043ea783f49fEnglishSymplectic ElementsIOP Publishing2020Thelen, AECordiner, MANixon, CAVuitton, VKisiel, ZCharnley, SBPalmer, MYTeanby, NAIrwin, PGJTitan harbors a dense, organic-rich atmosphere primarily composed of N2 and CH4, with lesser amounts of hydrocarbons and nitrogen-bearing species. As a result of high-sensitivity observations by the Atacama Large Millimeter/submillimeter Array (ALMA) in Band 6 (∼230–272 GHz), we obtained the first spectroscopic detection of CH3C3N (methylcyanoacetylene or cyanopropyne) in Titan's atmosphere through the observation of seven transitions in the $J=64\to 63$ and $J=62\to 61$ rotational bands. The presence of CH3C3N on Titan was suggested by the Cassini Ion and Neutral Mass Spectrometer detection of its protonated form: C4H3NH+, but the atmospheric abundance of the associated (deprotonated) neutral product is not well constrained due to the lack of appropriate laboratory reaction data. Here, we derive the column density of CH3C3N to be (3.8–5.7) × 1012 cm−2 based on radiative transfer models sensitive to altitudes above 400 km Titan's middle atmosphere. When compared with laboratory and photochemical model results, the detection of methylcyanoacetylene provides important constraints for the determination of the associated production pathways (such as those involving CN, CCN, and hydrocarbons), and reaction rate coefficients. These results also further demonstrate the importance of ALMA and (sub)millimeter spectroscopy for future investigations of Titan's organic inventory and atmospheric chemistry, as CH3C3N marks the heaviest polar molecule detected spectroscopically in Titan's atmosphere to date. |
| spellingShingle | Thelen, AE Cordiner, MA Nixon, CA Vuitton, V Kisiel, Z Charnley, SB Palmer, MY Teanby, NA Irwin, PGJ Detection of CH3C3N in Titan's atmosphere |
| title | Detection of CH3C3N in Titan's atmosphere |
| title_full | Detection of CH3C3N in Titan's atmosphere |
| title_fullStr | Detection of CH3C3N in Titan's atmosphere |
| title_full_unstemmed | Detection of CH3C3N in Titan's atmosphere |
| title_short | Detection of CH3C3N in Titan's atmosphere |
| title_sort | detection of ch3c3n in titan s atmosphere |
| work_keys_str_mv | AT thelenae detectionofch3c3nintitansatmosphere AT cordinerma detectionofch3c3nintitansatmosphere AT nixonca detectionofch3c3nintitansatmosphere AT vuittonv detectionofch3c3nintitansatmosphere AT kisielz detectionofch3c3nintitansatmosphere AT charnleysb detectionofch3c3nintitansatmosphere AT palmermy detectionofch3c3nintitansatmosphere AT teanbyna detectionofch3c3nintitansatmosphere AT irwinpgj detectionofch3c3nintitansatmosphere |