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Interpretation of the carbon abundance in Saturn measured by Cassini

机译:卡西尼号解释的土星碳丰度

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Spectral observations of Saturn from the far infrared spectrometer aboard the Cassini spacecraft [Flasar, F.M., et al., 2005. Temperatures, winds, and composition in the Saturnian system. Science 307, 1247-1251] have revealed that the C/H ratio in the planet is in fact about twice higher than previously derived from ground based observations and in agreement with the C/H value derived from Voyager IRIS by Courtin et al. [1984. The composition of Saturn's atmosphere at northern temperate latitudes from Voyager IRIS spectra - NH_3, PH_3, C_2H_2, C_2H_6, CH_3D, CH_4, and the Saturnian D/H isotopic ratio. Astrophys. J. 287, 899-916]. The implications of this measurement are reanalyzed in the present report on the basis that volatiles observed in cometary atmospheres, namely CO_2, CH_4, NH_3 and H_2S may have been trapped as solids in the feeding zone of the planet. CH_4 and H_2S may have been in the form of clathrate hydrates while CO_2 presumably condensed in the cooling solar nebula. Carbon may also have been incorporated in organics. Conditions of temperature and pressure ease the hydratation of NH_3. Such icy grains were included in planetesimals which subsequently collapsed into the hydrogen envelope of the planet, then resulting in C, N and S enrichments with respect to the solar abundance. Our calculations are consistent, within error bars, with observed elemental abundances on Saturn provided that the carbon trapped in planetesimals was mainly in the form of CH_4 clathrate and CO_2 ice (and maybe as organics) while nitrogen was in the form of NH_3 hydrate. Our approach has implications on the possible pattern of noble gases in Saturn, since we predict that contrary to what is observed in Jupiter, Ar and Kr should be in solar abundance while Xe might be strongly oversolar. The only way to verify this scenario is to send a probe making in situ mass spectrometer measurements. Our scenario also predicts that the ~(14)N/~(15)N ratio should be somewhat smaller in Saturn than measured in Jupiter by Galileo.
机译:卡西尼号飞船上的远红外光谱仪对土星的光谱观测[Flasar,F.M.等人,2005年。土星系统中的温度,风和成分。 [科学307,1247-1251]揭示了行星中的C / H比值实际上比以前从地面观测获得的C / H值高出大约两倍,并且与Courtin等人从旅行者IRIS得出的C / H值一致。 [1984年。根据旅行者IRIS光谱-NH_3,PH_3,C_2H_2,C_2H_6,CH_3D,CH_4和土星D / H同位素比,北温带纬度土星大气的组成。天体。 J. 287,899-916]。在本报告中,基于在彗星大气中观察到的挥发物,即CO_2,CH_4,NH_3和H_2S可能已作为固体被捕集在行星的进食区中,在此报告中重新分析了这种测量的含义。 CH_4和H_2S可能是笼形水合物的形式,而CO_2可能在冷却的太阳星云中冷凝。碳也可能已掺入有机物中。温度和压力条件减轻了NH_3的水合。这样的冰粒包含在小行星中,随后坍塌进入行星的氢层,然后导致相对于太阳丰度的C,N和S富集。我们的计算在误差棒内与观测到的土星上的元素丰度是一致的,前提是在小行星中捕获的碳主要以CH_4包合物和CO_2冰的形式存在(可能是有机物),而氮以NH_3水合物的形式存在。我们的方法对土星中可能存在的稀有气体模式具有影响,因为我们预测与木星中观察到的相反,Ar和Kr应该处于太阳丰度,而Xe可能强烈过太阳。验证这种情况的唯一方法是发送探针进行原位质谱仪测量。我们的情景还预测,土星的〜(14)N /〜(15)N比应该比伽利略在木星中测量的要小。

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