Ozone abundance on Mars from infrared heterodyne spectra II.: Validating photochemical models
Ozone abundance on Mars from infrared heterodyne spectra II.: Validating photochemical models
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DOI：
10.1016/j.icarus.2006.03.012
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发表时间：
2006-08-01
期刊：
影响因子：
3.2
通讯作者：
Lefevre, Franck
中科院分区：
文献类型：
--
作者：
Fast, Kelly;Kostiuk, Theodor;Lefevre, Franck
臭氧是火星光化学中一种重要的可观测示踪剂。包括对火星大气的化学和稳定性很重要的奇氢（HOx）。光谱分辨率>= 10(6)的红外外差光谱提供了火星大气中臭氧吸收特征的唯一地面直接途径。臭氧丰度是用戈达德红外外差光谱仪和位于夏威夷莫纳克亚山的美国宇航局红外望远镜设施的行星风和成分外差仪器测量的。从不同纬度和轨道位置（L-S = 40度，74度，102度，115度，202度，208度，291度）获取的总臭氧柱丰度与火星大气的第一个三维气相光化学模型[Lefevre]预测的结果进行了比较。F, Lebonnois， S, Montmessin， F, Forget， F, 2004。j .地球物理学。Res. 109, doi: 10.1029/2004JE002268。E07004]。观测到的和模拟的臭氧丰度在所有纬度的近日点轨道位置（LS = 202度，208度，291度）显示出良好的一致性。在远日点轨道位置（L-S = 40°，74°，115°）观测到的低纬度臭氧丰度显著高于模型预测的臭氧丰度。奇怪的氢在水冰云粒子上的不均匀损失可以解释这种差异，因为在火星远日点附近的低纬度地区可以观察到云。(c) 2006爱思唯尔公司版权所有。
Ozone is an important observable tracer of martian photochemistry. including odd hydrogen (HOx) species important to the chemistry and stability of the martian atmosphere. Infrared heterodyne spectroscopy with spectral resolution >= 10(6) provides the only ground-based direct access to ozone absorption features in the martian atmosphere. Ozone abundances were measured with the Goddard Infrared Heterodyne Spectrometer and the Heterodyne Instrument for Planetary Wind and Composition at the NASA Infrared Telescope Facility on Mauna Kea, Hawai'i. Retrieved total ozone column abundances from various latitudes and orbital positions (L-S = 40 degrees, 74 degrees, 102 degrees, 115 degrees, 202 degrees, 208 degrees, 291 degrees) are compared to those predicted by the first three-dimensional gas phase photochemical model of the martian atmosphere [Lefevre. F., Lebonnois, S., Montmessin, F., Forget, F., 2004. J. Geophys. Res. 109, doi: 10.1029/2004JE002268. E07004]. Observed and modeled ozone abundances show good agreement at all latitudes at perihelion orbital positions (LS = 202 degrees, 208 degrees, 291 degrees). Observed low-latitude ozone abundances are significantly higher than those predicted by the model at aphelion orbital positions (L-S = 40 degrees, 74 degrees, 115 degrees). Heterogeneous loss of odd hydrogen onto water ice cloud particles would explain the discrepancy, as clouds are observed at low latitudes around aphelion on Mars. (c) 2006 Elsevier Inc. All rights reserved.