Analytic investigation of climate stability on Titan: sensitivity to volatile inventory     

Ralph D. Lorenz  Christopher P. McKay  Jonathan I. Lunine 《Planetary and Space Science》1999,47(12):1503-1515

We develop a semiempirical grey radiative model to quantify Titan’s surface temperature as a function of pressure and composition of a nitrogen-methane-hydrogen atmosphere, solar flux and atmospheric haze. We then use this model, together with non-ideal gas-liquid equilibrium theory to investigate the behavior of the coupled surface-atmosphere system on Titan. We find that a volatile-rich Titan is unstable with respect to a runaway greenhouse—small increases in solar luminosity from the present value can lead to massive increases in surface temperature. If methane has been photolyzed throughout Titan’s history, then this runaway can only be avoided if the photolytic ethane is removed from the surface-atmosphere system.  相似文献   

William A. Cassidy (1928–2020)     

John Schutt  Ralph Harvey  Christian Koeberl 《Meteoritics & planetary science》2020,55(7):1709-1712

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Reflectance spectroscopy of insoluble organic matter (IOM) and carbonaceous meteorites     

Hannah H. Kaplan  Ralph E. Milliken  Conel M. O'D. Alexander  Christopher D. K. Herd 《Meteoritics & planetary science》2019,54(5):1051-1068

Insoluble organic matter (IOM) is the major organic component of chondritic meteorites and may be akin to organic materials from comets and interplanetary dust particles (IDPs). Reflectance spectra of IOM in the range 0.35–25 μm are presented as a tool for interpreting organic chemistry from remote measurements of asteroids, comets, IDPs, and other planetary bodies. Absorptions in the IOM spectra were strongly related to elemental H/C (atom) ratio. The aliphatic 3.4 μm absorption in IOM spectra increased linearly in strength with increasing H/C for H/C > 0.4, but was absent at lower H/C values. When meteorite spectra from the Reflectance Experiment Laboratory (RELAB) spectral catalog (n = 85) were reanalyzed at 3.4 μm, this detection limit (H/C > 0.4) persisted. Aromatic absorption features seen in IOM spectra were not observed in the meteorite spectra due to overlapping absorptions. However, the 3.4 μm aliphatic absorption strength for the bulk meteorites was correlated with both H/C of the meteorite's IOM and bulk C (wt%). Gaussian modeling of the 3 μm region provided an additional estimate of bulk C for the meteorites, along with bulk H (wt%), which is related to phyllosilicate abundance. These relationships lay the foundation for determining organic and phyllosilicate abundances from reflectance spectra. Both the full IOM spectra and the spectral parameters discussed here will aid in the interpretation of data from asteroid missions (e.g., OSIRIS‐REx, Hayabusa2), and may be able to place unknown spectral samples within the context of the meteorite collection.  相似文献   

三维正交非结构网格数值模型中物理流场的定义方法与改进     

刘晓辉  董礼先  Ralph T. Cheng 《海洋与湖沼》2010,41(4):621-627

使用Casulli等(2000)的数值方法建立了基于正交非结构网格的U型渠道的三维近岸正压水动力数值模型,检验了模型使用ELM(Eulerian-Lagrangian Method)方法处理平流项时,物理流场的定义对模拟结果的作用。数值试验和结果分析说明,使用ELM方法计算平流项所需的物理流场对计算结果影响明显,而目前常用的两种物理流场定义方法都存在一定不足——水位计算值对流速变化的反映不灵敏或者会产生小扰动等。针对常用物理流场定义方法的不足之处,作者在Casulli方法的基础上利用对多边形切向流速分量进行平均的方法改进了物理流场定义,抑制了小扰动。  相似文献   

A photogrammetric surveying method for field applications     

Dirk H.  Rieke-Zapp  Ralph  Rosenbauer  Fritz  Schlunegger 《The Photogrammetric Record》2009,24(125):5-22

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