Variability of phosphine on Jupiter from 5-μm spectroscopy     

Pierre Drossart  Thérèse Encrenaz  Alan T. Tokunaga 《Icarus》1984,60(3):613-620

Spectra of Jupiter recorded in the 1900- to 2300-cm^?1 range at the IRTF in Hawaii, July 1982, provide tentative evidence for variability of the Jovian atmosphere between zones and belts. It is concluded from analysis of the ν₁and ν₃ bands of PH₃ that there is a possible enhancement of the PH₃/H₂ ratio in the belts when compared to the zones. There is an apparent reduction of the PH₃ abundance between the IRIS Voyager 1 determinations and these spectra, implying temporal or spatial variability of PH₃ on Jupiter. Interpretation of this variability in the troposphere could involve both dynamical and thermochemical processes.  相似文献   

Recommended Sampling Intervals for Arsenic in Private Wells     

Brian J. Mailloux  Nicholas A. Procopio  Mark Bakker  Therese Chen  Imtiaz Choudhury  Kazi Matin Ahmed  M. Rajib H. Mozumder  Tyler Ellis  Steve Chillrud  Alexander van Geen 《Ground water》2021,59(1):80-89

Geogenic arsenic in drinking water is a worldwide problem. For private well owners, testing (e.g., private or government laboratory) is the main method to determine arsenic concentration. However, the temporal variability of arsenic concentrations is not well characterized and it is not clear how often private wells should be tested. To answer this question, three datasets, two new and one publicly available, with temporal arsenic data were utilized: 6370 private wells from New Jersey tested at least twice since 2002, 2174 wells from the USGS NAWQA database, and 391 private wells sampled 14 years apart from Bangladesh. Two arsenic drinking water standards are used for the analysis: 10 µg/L, the WHO guideline and EPA standard or maximum contaminant level (MCL) and 5 µg/L, the New Jersey MCL. A rate of change was determined for each well and these rates were used to predict the temporal change in arsenic for a range of initial arsenic concentrations below an MCL. For each MCL and initial concentration, the probability of exceeding an MCL over time was predicted. Results show that to limit a person to below a 5% chance of drinking water above an MCL, wells that are ½ an MCL and above should be tested every year and wells below ½ an MCL should be tested every 5 years. These results indicate that one test result below an MCL is inadequate to ensure long-term compliance. Future recommendations should account for temporal variability when creating drinking water standards and guidance for private well owners.  相似文献   

Hydrochemical assessment of pond and stream water near abandoned barite mine sites in parts of Oban massif and Mamfe Embayment,Southeastern Nigeria   总被引：1，自引：1，他引：0  

Christopher Iorfa Adamu  Therese Nganje  Aniekan Edet 《Environmental Earth Sciences》2014,71(9):3793-3811

Hydrochemical studies were carried out in parts of Oban Massif and Mamfe Embayment, Southeastern Nigeria to examine the contributions of barite mining activities on water quality. Pond and stream water samples were collected from six abandoned barite mines and adjoining streams areas during dry and wet seasons. These samples were analysed for physicochemical parameters using standard techniques. The results showed that the quality of water samples in the vicinity of barite mine sites was characterized by low pH, low mineralization, high suspended solids and deep colour. Sodium (Na⁺) and calcium (Ca²⁺) are the dominant cations and bicarbonate (HCO₃ ^?) and sulphate (SO₄ ^2?) the dominant anions. The low concentration of dissolved silica, relatively high concentrations of Na⁺, HCO₃ ^? and SO₄ ^2? suggest a combined influence of silicate, carbonate and weathering of mine spoils. The total dissolved solids, total suspended solids, electrical conductivity and major ions (except Na⁺ and K⁺) are higher for water draining barite mines from Cretaceous sediments, while Na⁺, K⁺, Ba²⁺ are higher in basement rock areas. Correlation and factor analyses suggest that the main components of the water samples are related to anthropogenic, geogenic, mineralization and environmental controls, while Gibbs diagram plots indicate weathering as the main process controlling the chemistry of water. Computed values of hardness and some irrigational parameters showed that the pond and stream water samples are generally soft and can be used for irrigation. Generally, the water quality satisfied the WHO (2008) and NIS (2007) standards for domestic, agriculture and industrial. However, there is the need to assess the impact of the pollution on the ecosystem and human health while remediation measures are being considered.  相似文献   

Observations of atmospheric water vapor above the Tharsis volcanoes on Mars with the OMEGA/MEx imaging spectrometer     

Luca Maltagliati  Dmitry V. Titov  Thérèse Encrenaz  Francois Forget  Horst U. Keller  Jean-Pierre Bibring 《Icarus》2008,194(1):53-64

The OMEGA imaging spectrometer onboard the Mars Express spacecraft is particularly well suited to study in detail specific regions of Mars, thanks to its high spatial resolution and its high signal-to-noise ratio. We investigate the behavior of atmospheric water vapor over the four big volcanoes located on the Tharsis plateau (Olympus, Ascraeus, Pavonis and Arsia Mons) using the 2.6 μm band, which is the strongest and most sensitive H₂O band in the OMEGA spectral range. Our data sample covers the end of MY26 and the whole MY27, with gaps only in the late northern spring and in northern autumn. The most striking result of our retrievals is the increase of water vapor mixing ratio from the valley to the summit of volcanoes. Corresponding column density is often almost constant, despite a factor of ∼5 decrease in air mass from the bottom to the top. This peculiar water enrichment on the volcanoes is present in 75% of the orbits in our sample. The seasonal distribution of such enrichment hints at a seasonal dependence, with a minimum during the northern summer and a maximum around the northern spring equinox. The enrichment possibly also has a diurnal trend, being the orbits with a high degree of enrichment concentrated in the early morning. However, the season and the solar time of the observations, due to the motion of the spacecraft, are correlated, then the two dependences cannot be clearly disentangled. Several orbits exhibit also spatially localized enrichment structures, usually ring- or crescent-shaped. We retrieve also the height of the saturation level over the volcanoes. The results show a strong minimum around the aphelion season, due to the low temperatures, while it raises quickly before and after this period. The enrichment is possibly generated by the local circulation characteristic of the volcano region, which can transport upslope significant quantities of water vapor. The low altitude of the saturation level during the early summer can then hinder the transport of water during this season. The influence of the coupling between atmosphere and surface, due mainly to the action of the regoliths, can also contribute partially to the observed phenomenon.  相似文献   

An estimate of the PH₃, CH₃D,and GeH₄ Abundances on Jupiter from the Voyager IRIS data at 4.5 μm     

P. Drossart  T. Encrenaz  V. Kunde  R. Hanel  M. Combes 《Icarus》1982,49(3):416-426

The abundances of PH₃, CH₃D, and GeH₄ are derived from the 2100- to 2250-cm^?1 region of the Voyager 1 IRIS spectra. No evidence is seen for large-scale variations of the phosphine abundance over Jovian latitudes between ?30 and +30°. In the atmospheric regions corresponding to 170–200°K, the derived PH₃/H₂ value is (4.5 ± 1.5) × 10^?7 or 0.75 ± 0.25 times the solar value. This result, compared with other PH₃ determinations at 10 μm, suggests than the PH₃/H₂ ratio on Jupiter decreases with atmospheric pressure. In the 200–250°K region, we derive, within a factor of 2, CH₃D/H₂ and GeH₄/H₂ ratios of 2.0 × 10^?7 and 1.0 × 10^?9, respectively. Assuming a C/H value of 1.0 × 10^?3, as derived from Voyager, our CH₃D/H₂ ratio implies a D/H ratio of 1.8 × 10^?5, in reasonable agreement with the interstellar medium value.  相似文献   

The Jovian spectrum in the 3-μm window     

Pierre Drossart  Thérèse Encrenaz 《Icarus》1983,55(3):390-398

The spectral window of Jupiter at 3 μm is analyzed and compared with previously published spectra. The two components of the spectrum, the thermal and the solar reflected contributions, are calculated at low resolution (30 cm^?1) between 3300 and 3800 cm^?1 for preparing the interpretation of the Galileo Near Infrared Mapping Spectrometer experiment. The calculations yield to the following conclusions: (1) NH₃ is the main absorber between 3300 and 3600 cm^?1 for both the thermal spectrum and the solar reflected spectrum; H₂O appears only in the thermal component above 3600 cm^?1. (2) The thermal component can be seen only on the dark side of Jupiter; the atmosphere is sounded down to temperature levels of about 210°K. (3) The solar reflected component can be modelized by a reflecting layer between 135 and 140°K with an albedo of 0.3; high spatial resolution maps of Jupiter at 3 μm should give access to the NH₃ spatial distribution on Jupiter.  相似文献   

Avoidance response of sediment living amphipods to zinc pyrithione as a measure of sediment toxicity     

Eriksson Wiklund AK  Börjesson T  Wiklund SJ 《Marine pollution bulletin》2006,52(1):96-99

An avoidance test was developed using non-cultured individuals of the sediment dwelling amphipod Monoporeia affinis. As test substance we used zinc pyrithione, an antifouling agent and a common shampoo ingredient. The toxicity to Daphnia and fish is well known but sediment toxicity of this very hydrophobic compound is less known. The preference of juvenile M. affinis was tested in jars, each including 12 petri dishes. In each replicate, half of the petri dishes contained sediment mixed with six concentrations ranging from 0 to 10microg zinc pyrithione per L sediment and half of the petri dishes contained the corresponding sediment-substance mixture plus an extra food addition. The amphipods significantly avoided petri dishes with the three highest concentrations of zinc pyrithione and the calculated EC(50) was 9.65microgL(-1) sediment. No difference in mortality was observed between concentrations. Using the avoidance behaviour in sediment toxicity testing is a simple and cost-effective screening for toxicants.  相似文献   

In memoriam Vasily Ivanovitch Moroz (1931-2004)     

Thérèse Encrenaz 《Planetary and Space Science》2004,52(14):1231-1232

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Call for Ph.D. abstracts in Planetary and Space Science     

Therese Encrenaz 《Planetary and Space Science》2006,54(1):1

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Compositional constraints on giant planet formation     

Tobias Owen  Therese Encrenaz 《Planetary and Space Science》2006,54(12):1188-1196

Using Ockham's razor as a guide, we have tried to find the simplest model for the formation of giant planets that can explain current observations of atmospheric composition. While this “top-down” approach is far from sufficient to define such models, it establishes a set of boundary conditions whose satisfaction is necessary. Using Jupiter as the prototype, we find that a simple model for giant planet formation that begins with a solar nebula of uniform composition and relies on accretion of low temperature icy planetesimals plus collapse of surrounding solar nebula gas supplies that satisfaction. We compare the resulting predictions of elemental abundances and isotope ratios in the atmospheres of the other giants with those from contrasting models and suggest some key measurements to make further progress.  相似文献