Infrared characterisation of acetonitrile and propionitrile aerosols under Titan's atmospheric conditions
Pure, crystalline acetonitrile (CH CN) and propionitrile (CH CH CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures to be compiled from 50 to 5000 cm . The cell temperature and pressure conditions were controlled to simulate Titan's lower atmosphere (80...
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| Published in | Physical chemistry chemical physics : PCCP Vol. 19; no. 4; pp. 2915 - 2925 |
|---|---|
| Main Authors | , , , |
| Format | Journal Article |
| Language | English |
| Published |
England
2017
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| Subjects | |
| Online Access | Get full text |
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| Abstract | Pure, crystalline acetonitrile (CH
CN) and propionitrile (CH
CH
CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures to be compiled from 50 to 5000 cm
. The cell temperature and pressure conditions were controlled to simulate Titan's lower atmosphere (80-130 K and 1-100 mbar), allowing for the comparison of laboratory data to the spectra obtained from the Cassini-Huygens mission. The far-IR features confirmed the morphology of CH
CN aerosols as the metastable β-phase (monoclinic) ice, however, a specific crystalline phase for CH
CH
CN could not be verified. Mie theory and the literature complex refractive indices enabled of the experimental spectra to be modelled. The procedure yielded size distributions for CH
CN (55-140 nm) and CH
CH
CN (140-160 nm) particles. Effective kinetic profiles, tracing the evolution of aerosol band intensities, showed that condensation of CH
CH
CN proceeded at twice the rate of CH
CN aerosols. In addition, the rate of CH
CH
CN aerosol depletion via lateral diffusion of the particles from the interrogation volume was approximately 50% faster than that of CH
CN. The far-IR spectra recorded for both nitrile aerosols did not display absorption profiles that could be attributed to the unassigned 220 cm
feature, which has been observed to fluctuate seasonally in the spectra obtained from Titan's atmosphere. |
|---|---|
| AbstractList | Pure, crystalline acetonitrile (CH3CN) and propionitrile (CH3CH2CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures to be compiled from 50 to 5000 cm-1. The cell temperature and pressure conditions were controlled to simulate Titan's lower atmosphere (80-130 K and 1-100 mbar), allowing for the comparison of laboratory data to the spectra obtained from the Cassini-Huygens mission. The far-IR features confirmed the morphology of CH3CN aerosols as the metastable beta -phase (monoclinic) ice, however, a specific crystalline phase for CH3CH2CN could not be verified. Mie theory and the literature complex refractive indices enabled of the experimental spectra to be modelled. The procedure yielded size distributions for CH3CN (55-140 nm) and CH3CH2CN (140-160 nm) particles. Effective kinetic profiles, tracing the evolution of aerosol band intensities, showed that condensation of CH3CH2CN proceeded at twice the rate of CH3CN aerosols. In addition, the rate of CH3CH2CN aerosol depletion via lateral diffusion of the particles from the interrogation volume was approximately 50% faster than that of CH3CN. The far-IR spectra recorded for both nitrile aerosols did not display absorption profiles that could be attributed to the unassigned 220 cm-1 feature, which has been observed to fluctuate seasonally in the spectra obtained from Titan's atmosphere. Pure, crystalline acetonitrile (CH 3 CN) and propionitrile (CH 3 CH 2 CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures to be compiled from 50 to 5000 cm −1 . The cell temperature and pressure conditions were controlled to simulate Titan's lower atmosphere (80–130 K and 1–100 mbar), allowing for the comparison of laboratory data to the spectra obtained from the Cassini–Huygens mission. The far-IR features confirmed the morphology of CH 3 CN aerosols as the metastable β-phase (monoclinic) ice, however, a specific crystalline phase for CH 3 CH 2 CN could not be verified. Mie theory and the literature complex refractive indices enabled of the experimental spectra to be modelled. The procedure yielded size distributions for CH 3 CN (55–140 nm) and CH 3 CH 2 CN (140–160 nm) particles. Effective kinetic profiles, tracing the evolution of aerosol band intensities, showed that condensation of CH 3 CH 2 CN proceeded at twice the rate of CH 3 CN aerosols. In addition, the rate of CH 3 CH 2 CN aerosol depletion via lateral diffusion of the particles from the interrogation volume was approximately 50% faster than that of CH 3 CN. The far-IR spectra recorded for both nitrile aerosols did not display absorption profiles that could be attributed to the unassigned 220 cm −1 feature, which has been observed to fluctuate seasonally in the spectra obtained from Titan's atmosphere. Pure, crystalline acetonitrile (CH CN) and propionitrile (CH CH CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures to be compiled from 50 to 5000 cm . The cell temperature and pressure conditions were controlled to simulate Titan's lower atmosphere (80-130 K and 1-100 mbar), allowing for the comparison of laboratory data to the spectra obtained from the Cassini-Huygens mission. The far-IR features confirmed the morphology of CH CN aerosols as the metastable β-phase (monoclinic) ice, however, a specific crystalline phase for CH CH CN could not be verified. Mie theory and the literature complex refractive indices enabled of the experimental spectra to be modelled. The procedure yielded size distributions for CH CN (55-140 nm) and CH CH CN (140-160 nm) particles. Effective kinetic profiles, tracing the evolution of aerosol band intensities, showed that condensation of CH CH CN proceeded at twice the rate of CH CN aerosols. In addition, the rate of CH CH CN aerosol depletion via lateral diffusion of the particles from the interrogation volume was approximately 50% faster than that of CH CN. The far-IR spectra recorded for both nitrile aerosols did not display absorption profiles that could be attributed to the unassigned 220 cm feature, which has been observed to fluctuate seasonally in the spectra obtained from Titan's atmosphere. Pure, crystalline acetonitrile (CH3CN) and propionitrile (CH3CH2CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures to be compiled from 50 to 5000 cm-1. The cell temperature and pressure conditions were controlled to simulate Titan's lower atmosphere (80-130 K and 1-100 mbar), allowing for the comparison of laboratory data to the spectra obtained from the Cassini-Huygens mission. The far-IR features confirmed the morphology of CH3CN aerosols as the metastable β-phase (monoclinic) ice, however, a specific crystalline phase for CH3CH2CN could not be verified. Mie theory and the literature complex refractive indices enabled of the experimental spectra to be modelled. The procedure yielded size distributions for CH3CN (55-140 nm) and CH3CH2CN (140-160 nm) particles. Effective kinetic profiles, tracing the evolution of aerosol band intensities, showed that condensation of CH3CH2CN proceeded at twice the rate of CH3CN aerosols. In addition, the rate of CH3CH2CN aerosol depletion via lateral diffusion of the particles from the interrogation volume was approximately 50% faster than that of CH3CN. The far-IR spectra recorded for both nitrile aerosols did not display absorption profiles that could be attributed to the unassigned 220 cm-1 feature, which has been observed to fluctuate seasonally in the spectra obtained from Titan's atmosphere. |
| Author | Ennis, C Robertson, E G Auchettl, R Ruzi, M |
| Author_xml | – sequence: 1 givenname: C orcidid: 0000-0003-1774-8982 surname: Ennis fullname: Ennis, C email: c.ennis@latrobe.edu.au organization: Department of Chemistry and Physics, La Trobe Institute for Molecular Science, La Trobe University, Victoria, 3086, Australia. c.ennis@latrobe.edu.au – sequence: 2 givenname: R surname: Auchettl fullname: Auchettl, R email: c.ennis@latrobe.edu.au organization: Department of Chemistry and Physics, La Trobe Institute for Molecular Science, La Trobe University, Victoria, 3086, Australia. c.ennis@latrobe.edu.au – sequence: 3 givenname: M surname: Ruzi fullname: Ruzi, M email: c.ennis@latrobe.edu.au organization: Department of Chemistry and Physics, La Trobe Institute for Molecular Science, La Trobe University, Victoria, 3086, Australia. c.ennis@latrobe.edu.au – sequence: 4 givenname: E G orcidid: 0000-0003-4346-4457 surname: Robertson fullname: Robertson, E G email: c.ennis@latrobe.edu.au organization: Department of Chemistry and Physics, La Trobe Institute for Molecular Science, La Trobe University, Victoria, 3086, Australia. c.ennis@latrobe.edu.au |
| BackLink | https://www.ncbi.nlm.nih.gov/pubmed/28079222$$D View this record in MEDLINE/PubMed |
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| Snippet | Pure, crystalline acetonitrile (CH
CN) and propionitrile (CH
CH
CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures... Pure, crystalline acetonitrile (CH 3 CN) and propionitrile (CH 3 CH 2 CN) particles were formed in a collisional cooling cell allowing for infrared (IR)... Pure, crystalline acetonitrile (CH3CN) and propionitrile (CH3CH2CN) particles were formed in a collisional cooling cell allowing for infrared (IR) signatures... |
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| SubjectTerms | Acetonitrile Aerosols Crystal structure Diffusion rate Infrared signatures Saturn satellites Spectra Titan |
| Title | Infrared characterisation of acetonitrile and propionitrile aerosols under Titan's atmospheric conditions |
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