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The three-micron spectral feature of the Saturnian haze: Implications for the haze composition and formation process

机译：土星雾度的三微米光谱特征：对雾度成分和形成过程的影响

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摘要

We retrieve a 3.4-μm spectral feature pertaining to the Saturnian haze from Cassini/VIMS Procyon occultation data obtained at 12 different altitudes from approximately 0.7 to 0.0018 mbar (Nicholson et al., 2006; Bellucci, 2008; Bellucci et al., 2009). The occultation occurred at 55°N latitude, at the edge of the "polar hood" region, where the extinction from stratospheric aerosols becomes strongest. The improved retrieval procedure eliminates the influence of strong adjacent CH_4 absorption bands. We derive optical-depth spectra (hereafter called τ-spectra) of the haze on a relative scale and find that the τ-spectra exhibit a broad opacity peak at 3.36-3.41 μm. At the 0.7-0.025 mbar levels, the opacity is maximum at 3.41 μm, which approximately coincides with the 3.4-μm aliphatic C-H stretching bands typical of the solid state of hydrocarbons such as C_5H_(12), C_6H_(12), C_6H_(14) and C_7H_(14), but not limited to these molecules. At the 0.015-0.0018 mbar levels, however, maximum opacity occurs at 3.36 um, similarly to the τ-spectra of Titan's haze (Kim et al., 2011), suggesting similar chemical composition and possibly a similar formation mechanism occurring in the upper stratospheres of Saturn and Titan. We also find that with mole fractions on the order of 1 ppb, C_6H_(12), C_6H_(14) and C_7H_(14) can be saturated near the lower levels of the occultation, suggesting that condensation of these or other heavier hydrocarbons could contribute to the formation of the stratospheric haze particles at these altitudes on Saturn.
机译：我们从在约0.7至0.0018 mbar的12个不​​同高度上获得的Cassini / VIMS Procyon掩星数据中检索到了一个与土星雾度有关的3.4μm光谱特征（Nicholson等，2006; Bellucci，2008; Bellucci等，2009） 。掩星发生在北纬55°，“极地罩”区域的边缘，平流层气溶胶的消光最强。改进的检索程序消除了强相邻CH_4吸收带的影响。我们在相对尺度上得出雾度的光学深度光谱（以下称为τ光谱），发现τ光谱在3.36-3.41μm处显示出较宽的不透明峰。在0.7-0.025 mbar的水平下，不透明度最大为3.41μm，大约与碳氢化合物固态C_5H_（12），C_6H_（12），C_6H_（14 ）和C_7H_（14），但不限于这些分子。然而，在0.015-0.0018 mbar的水平上，最大不透明性发生在3.36 um处，与土卫六的霾的τ谱相似（Kim等，2011），这表明在平流层上部存在相似的化学组成和可能的相似形成机制土星和土卫六。我们还发现，摩尔分数约为1 ppb时，C_6H_（12），C_6H_（14）和C_7H_（14）可以在较低的掩星水平附近饱和，这表明这些或其他较重烃的缩合可能会导致在土星上这些高度的平流层雾状颗粒的形成。

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  • 来源
    《Planetary and space science》 |2012年第1期|p.122-129|共8页
  • 作者

    S.J. Kim; C.K. Sim; D.W. Lee; R. Courtin; J.I. Moses; Y.C. Minh;

  • 作者单位

    School of Space Research, Kyung Hee University, Yongin 446-701, Republic of Korea;

    School of Space Research, Kyung Hee University, Yongin 446-701, Republic of Korea;

    School of Space Research, Kyung Hee University, Yongin 446-701, Republic of Korea;

    LESIA-Observatoire de Paris, CNRS, UPMC Univ. Paris 6, Univ. Paris-Diderot, 92195 Meudon, France;

    Space Science Institute, 4750 Walnut St, Suite 205, Boulder, CO 80301, USA;

    Korea Astronomy and Space Science Institute, Daejeon 305-348, Republic of Korea;

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  • 正文语种 eng
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  • 关键词

    saturn; atmosphere; haze; composition; infrared spectroscopy;

    机译：土星大气层;阴霾;组成;红外光谱;

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