Non-LTE radiative transfer for sub-millimeter water lines in Comet 67P/Churyumov-Gerasimenko     

Seungwon Lee  Paul von Allmen  Samuel Gulkis 《Icarus》2011,215(2):721-731

The European Space Agency (ESA) Rosetta spacecraft (Schulz, R., Alexander, C., Boehnhardt, H., Glassmeier, K.H. (Eds.) [2009]. “ROSETTA - ESA”) will encounter Comet 67P/Churyumov-Gerasimenko in 2014 and spend the next 18 months in the vicinity of the comet, permitting very high spatial and spectral resolution observations of the coma and nucleus. During this time, the heliocentric distance of the comet will change from ∼3.5 AU to ∼1.3 AU, accompanied by an increasing temperature of the nucleus and the development of the coma. The Microwave Instrument for the Rosetta Orbiter (MIRO) will observe the ground-state rotational transition (1₁₀-1₀₁) of H₂¹⁶O at 556.936 GHz, the two isotopologues H₂¹⁷O and H₂¹⁸O and other molecular transitions in the coma during this time (Gulkis, S. et al., [2007]. MIRO: Microwave Instrument for Rosetta Orbiter. Space Sci. Rev. 128, 561-597).The aim of this study is to simulate the water line spectra that could be obtained with the MIRO instrument and to understand how the observed line spectra with various viewing geometries can be used to study the physical conditions of the coma and the water excitation processes throughout the coma. We applied an accelerated Monte Carlo method to compute the excitations of the seven lowest rotational levels (1₀₁, 1₁₀, 2₁₂, 2₂₁, 3₀₃, 3₁₂, and 3₂₁) of ortho-water using a comet model with spherically symmetric water outgassing, density, temperature and expansion velocity at three different heliocentric distances 1.3 AU, 2.5 AU, and 3.5 AU. Mechanisms for the water excitation include water-water collisions, water-electron collisions, and infrared pumping by solar radiation.Synthetic line spectra are calculated at various observational locations and directions using the MIRO instrument parameters. We show that observations at varying viewing distances from the nucleus and directions have the potential to give diagnostic information on the continuum temperature and water outgassing rates at the surface of the nucleus, and the gas density, expansion velocity, and temperature of the coma as a function of distance from the nucleus. The gas expansion velocity and temperature affect the spectral line width and frequency shift of the line from the rest frequency, while the gas density (which is directly related to the outgassing rate) and the line excitation temperature determine the antenna temperature of the absorption and emission signal in the line profile.  相似文献   

Saturn’s tropospheric composition and clouds from Cassini/VIMS 4.6-5.1 μm nightside spectroscopy     

Leigh N. Fletcher  Kevin H. Baines  Adam P. Showman  Glenn S. Orton  C. Merlet 《Icarus》2011,214(2):510-533

The latitudinal variation of Saturn’s tropospheric composition (NH₃, PH₃ and AsH₃) and aerosol properties (cloud altitudes and opacities) are derived from Cassini/VIMS 4.6-5.1 μm thermal emission spectroscopy on the planet’s nightside (April 22, 2006). The gaseous and aerosol distributions are used to trace atmospheric circulation and chemistry within and below Saturn’s cloud decks (in the 1- to 4-bar region). Extensive testing of VIMS spectral models is used to assess and minimise the effects of degeneracies between retrieved variables and sensitivity to the choice of aerosol properties. Best fits indicate cloud opacity in two regimes: (a) a compact cloud deck centred in the 2.5-2.8 bar region, symmetric between the northern and southern hemispheres, with small-scale opacity variations responsible for numerous narrow light/dark axisymmetric lanes; and (b) a hemispherically asymmetric population of aerosols at pressures less than 1.4 bar (whose exact altitude and vertical structure is not constrained by nightside spectra) which is 1.5-2.0× more opaque in the summer hemisphere than in the north and shows an equatorial maximum between ±10° (planetocentric).Saturn’s NH₃ spatial variability shows significant enhancement by vertical advection within ±5° of the equator and in axisymmetric bands at 23-25°S and 42-47°N. The latter is consistent with extratropical upwelling in a dark band on the poleward side of the prograde jet at 41°N (planetocentric). PH₃ dominates the morphology of the VIMS spectrum, and high-altitude PH₃ at p < 1.3 bar has an equatorial maximum and a mid-latitude asymmetry (elevated in the summer hemisphere), whereas deep PH₃ is latitudinally-uniform with off-equatorial maxima near ±10°. The spatial distribution of AsH₃ shows similar off-equatorial maxima at ±7° with a global abundance of 2-3 ppb. VIMS appears to be sensitive to both (i) an upper tropospheric circulation (sensed by NH₃ and upper-tropospheric PH₃ and hazes) and (ii) a lower tropospheric circulation (sensed by deep PH₃, AsH₃ and the lower cloud deck).  相似文献   

A high-amplitude thermal inertia anomaly of probable magnetospheric origin on Saturn’s moon Mimas     

C.J.A. Howett  J.R. Spencer  R.E. Johnson  T.A. Hurford  M. Segura 《Icarus》2011,216(1):221-226

Spectral maps of Mimas’ daytime thermal emission show a previously unobserved thermal anomaly on Mimas’ surface. A sharp V-shaped boundary, centered at 0°N and 180°W, separates relatively warm daytime temperatures from a cooler anomalous region occupying low- to mid-latitudes on the leading hemisphere. Subsequent observations show the anomalous region is also warmer than its surroundings at night, indicating high thermal inertia. Thermal inertia in the anomalous region is , compared to < outside the anomaly. Bolometric Bond albedos are similar between the two regions, in the range 0.49-0.70. The mapped portion of the thermally anomalous region coincides in shape and location to a region of high-energy electron deposition from Saturn’s magnetosphere, which also has unusually high near-UV reflectance. It is therefore likely that high-energy electrons, which penetrate Mimas’ surface to the centimeter depths probed by diurnal temperature variations, also alter the surface texture, dramatically increasing its thermal inertia.  相似文献   

H₂O₂ production by high-energy electrons on icy satellites as a function of surface temperature and electron flux     

Kevin P. Hand  Robert W. Carlson 《Icarus》2011,215(1):226-233

Chemistry on the icy surface of Europa is heavily influenced by the incident energetic particle flux from the jovian magnetosphere. The majority (>75%) of this energy is in the form of high energy electrons (extending to >10 MeV). We have simulated the electron irradiation environment of Europa with a vacuum system containing a high-energy electron gun for irradiation of ice samples formed on a gold mirror cooled with a cryostat. Pure water films of ∼2.6 μm thickness were grown at 100 K and then either cooled (to 80 K), warmed (to 120 K) or left at 100 K and subsequently irradiated with 10 keV electrons. The production of hydrogen peroxide (H₂O₂) was monitored by observation of the 2850 cm⁻¹ (3.5 μm) band. Equilibrium concentrations of H₂O₂, in units of percent by number H₂O₂ relative to water, were found to be 0.043% (80 K), 0.029% (100 K), and 0.0063% (120 K). These values are 33%, 22%, and 5%, respectively, that of the reported surface concentration on the leading hemisphere of Europa (Carlson, R.W., Anderson, M.S., Johnson, R.E., Smythe, W.D., Hendrix, A.R., Barth, C.A., et al. [1999]. Science 283(5410), 2062-2064) and less than the equilibrium concentrations formed by ion irradiation. In addition to the ice film temperature, the current of electrons was varied between different experiments to determine the production and destruction of H₂O₂ as a function of both electron flux and ice temperature. Variation in current was found to have little effect on the results other than accelerating arrival at radiolytic equilibrium.  相似文献   

河套盆地周缘泉水化学组分对2015年4月15日阿左旗M_S5.8地震的响应^*     

孙凤霞  崔月菊  郑红巍  王玥  李继成  司学芸  李新艳  杜建国 《地震》2016,36(2):105-118

根据河套盆地周缘断裂带泉水的氢、氧同位素组成和水化学组分,讨论了该区地下水的化学类型、成因及其与地震活动的关系。于2014年9月下旬和2015年4月15日M_S5.8阿左旗地震震后在河套盆地周缘的乌拉山断裂带、色尔腾断裂带、狼山断裂带以及桌子山断裂带采集了17个泉水和井水样品,测得水样的TDS分布在143.8~42 553.0mg/L范围内,δD和δ¹⁸O值分别在-83.6‰~66.56‰和-11.16‰~8.2‰的范围内,来源为大气降水。根据舒卡列夫分类法,震前水样可划分为13种水化学类型,震后西山咀、圐圙朴隆等5个点采样点泉水的水化学类型发生变化。其中,乌拉山断裂带的水样以HCO₃-Ca型低矿化度地表水为主;色尔腾断裂带、狼山断裂带泉水受白垩系含水层影响,矿化度较高,富含HCO^-₃及SO^2-₄;桌子山一带受煤矿开采影响,水样以富SO^2-₄和Cl^-的高矿化度水为特征。地震前后TDS、阴、阳离子以及γNa/γCl、γ(SO₄+Cl)/γHCO₃、γHCO₃/γCl等毫克当量比值能够较好地反映地震。2015年4月15日阿左旗M_S5.8地震后,呼鲁斯太、迪延阿贵庙及八一井的水化学组成变化较大,对地震响应较为敏感。呼鲁斯太地区泉水的TDS稍有降低,但HCO^-₃在阴离子中所占比例有所增加,表明震后该地区含水层的泉水与较低矿化度的含碳酸盐岩含水层水发生了混合;八一井的TDS值有所增加,γNa/γCl比值有所降低,表明深部高矿化度水的混入;迪延阿贵庙水样的TDS稍有下降,但NaCl的相对含量较震前有所升高,表明有低矿化度NaCl水的混入。本工作不仅确定了该区水文地球化学背景,而且对地震监测和预测具有一定参考价值。  相似文献   

张掖盆地水文地质特征与稳定同位素研究   总被引：1，自引：0，他引：1  

张徽  安永会  韩双宝  何锦  李旭峰 《地下水》2009,31(6):123-125

论述了张掖盆地地下水赋存分布特征与地下水补给、径流、排泄条件,利用水化学、同位素调查的方法,重点对张掖甘州平原区地下水水化学类型及其演化过程进行了研究。结果表明：张掖盆地由源于南部祁连山和北部龙首山的水系沉积物组成,其冲洪积平原规模、含水层富水性、导水性与地下水水化学特征等方面存在差异;同时地下水稳定同住素特征分析印证了水文地质条件的差异。祁连山前沉积物与龙首山前沉积物中地下水有着不同的补给来源和径流路径。浅层地下水和龙首山前深层承压水主要补给源为大气降水和山区河流入渗补给,祁连山前深层承压地下水系统可能有冰雪融水补给。  相似文献   

黄土碳酸盐碳同位素环境意义讨论          下载免费PDF全文

金雅琪  苗甜  路珂珂  杨雁鹏  梁孔秋  宋垠先  陈忠 《盐湖研究》2022,30(1):87-94

黄土碳酸盐碳同位素广泛应用于第四纪气候环境变化的研究中,以往研究中多利用钙结核、次生碳酸盐或成壤碳酸盐,认为其反映了C4植物的丰度.黄土高原碳酸盐碳同位素表现为黄土层高,古土壤层中低,即黄土层中C4植物丰度高于古土壤层.然而,这样的结果和黄土有机碳同位素得到的结果矛盾,有机碳同位素的结果表明温度对C4植物的分布起到了决...  相似文献   

Lunar atmospheric H₂ detections by the LAMP UV spectrograph on the Lunar Reconnaissance Orbiter     

S. Alan Stern  Jason C. Cook  Jean -Yves Chaufray  Paul D. Feldman  G. Randall Gladstone  Kurt D. Retherford 《Icarus》2013

We report on the detection of H₂ as seen in our analysis of twilight observations of the lunar atmosphere observed by the LAMP instrument aboard NASA’s Lunar Reconnaissance Orbiter. Using a large amount of data collected on the lunar atmosphere between September 2009 and March 2013, we have detected and identified, the presence of H₂ in the native lunar atmosphere, for the first time. We derive a surface density for H₂ of 1.2 ± 0.4 × 10³ cm⁻³ at 120 K. This is about 10 times smaller than originally predicted, and several times smaller than previous upper limits from the Apollo era data.  相似文献   

Comparison of the moments of the Xmax distribution predicted by different cosmic ray shower simulation models     

《Astroparticle Physics》2013

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补水溶矿过程中达布逊湖北岸地下卤水水化学变化特征初步研究          下载免费PDF全文

李梦玲  袁小龙  张西营  苗卫良  洪荣昌  朱海霞  陈亮 《盐湖研究》2022,30(2):99-109

以察尔汗盐湖达布逊区段补水溶采区为研究区,靠近补水渠的D01、D03以及D05水文观测孔地下卤水为研究对象,通过水化学、相图等分析方法,研究了地下卤水在固液转化过程中水化学的时空变化特征及其影响因素。研究结果表明,储卤层中卤水化学特性在空间上具有明显差异性。在纵向上,随深度增加Na⁺、SO₄2-浓度、pH值降低,而Mg²⁺、Cl-、HCO₃-、Li⁺、B³⁺浓度、TDS和比重升高;在横向上,D01孔中卤水具有较高的Na⁺、SO₄2-、HCO₃-、Li⁺浓度、pH值以及较低的TDS和比重;D03孔中卤水具有较高的K⁺、B³⁺浓度;D05孔中具有较高的TDS、比重、Mg²⁺、Ca²⁺、Cl-以及Sr²⁺浓度。揭示了卤水在盐层中的滞留时间、盐层渗透性差异、矿物组合与分布及温度变化是影响地下卤水水化学分布特征的主要因素,并初步研究认为补水溶矿具有局限性,D01孔受补水影响最大,D03孔次之,D05孔受补水影响较弱。  相似文献