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Hydroxyl airglow on Venus in comparison with Earth

机译:金星上的羟基气辉与地球相比

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Hydroxyl nightglow is intensively studied in the Earth atmosphere, due to its coupling to the ozone cycle. Recently, it was detected for the first time also in the Venus atmosphere, thanks to the VIRTIS-Venus Express observations. The main △v=l, 2 emissions in the infrared spectral range, centred respectively, at 2.81 and 1.46 μm (which correspond to the (1-0) and (2-0) transitions, respectively), were observed in limb geometry (Piccioni et al., 2008) with a mean emission rate of 880 + 90 and 100 ± 40 kR (1 R= 10~6 photon cm~(-2) s~(-1) (4πster)~(-1)), respectively, integrated along the line of sight In this investigation, the Bates-Nicolet chemical reaction is reported to be the most probable mechanism for OH production on Venus, as in the case of Earth, but HO_2 and 0 may still be not negligible as mechanism of production for OH, differently than Earth. The nightglow emission from OH provides a method to quantif O_3, HO_2, H and O, and to infer the mechanism of transport of the key species involved in the productior Very recently, an ozone layer was detected in the upper atmosphere of Venus by the SPICAV (Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus) instrument onboard Venus Expres (Montmessin et al, 2009); this discovery enhances the importance of ozone to the OH production in the upper atmosphere of Venus through the Bates-Nicolet mechanism. On Venus, OH airglow is observed only in the night side and no evidence has been found whether a similar emission exists also in the day side. On Mars it is expected to exist both on the day and night sides of the planet, because of the presence of ozone though OH airglow has not yet been detected. In this paper, we review and compare the OH nightglow on Venus and Earth. The case of Mars is also briefly discussed for the sake of completeness. Similarities from a chemical and a dynamical point of view are listed, though visible OH emissions on Earth and IR OH emissions on Venus are compared.
机译:由于其与臭氧循环的耦合,人们在地球大气层中对羟丙基夜光进行了深入研究。最近,由于VIRTIS-Venus Express的观测,它也是在金星大气中首次被检测到。在肢体几何结构中观察到主要的△v = l,在红外光谱范围内有2个发射,分别位于2.81和1.46μm(分别对应于(1-0)和(2-0)过渡)。 Piccioni et al。,2008)的平均发射率为880 + 90和100±40 kR(1 R = 10〜6光子cm〜(-2)s〜(-1)(4πster)〜(-1))分别沿着视线进行整合在这项研究中,据报道,贝茨-尼科莱特化学反应是金星上产生OH的最可能机制,就像地球一样,但HO_2和0仍然可以忽略不计与地球不同的OH产生机理。 OH产生的夜辉发光提供了一种定量O_3,HO_2,H和O的方法,并可以推断出生产中涉及的关键物质的迁移机理。 (金星大气特征的光谱学研究)仪器在金星表达上(Montmessin et al,2009);这一发现通过Bates-Nicolet机制增强了臭氧对金星高层大气中OH产生的重要性。在金星上,仅在夜间观察到OH气辉,没有证据表明在白天也存在类似的排放。在火星上,由于臭氧的存在,尽管尚未发现OH气辉,但预计它会存在于行星的白天和夜晚。在本文中,我们回顾并比较了金星和地球上的OH夜光。为了完整起见,还简要讨论了火星的情况。从化学和动力学角度列出了相似之处,尽管比较了地球上的可见OH排放量和金星上的IR OH排放量。

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