Ion Densities in the Nightside Ionosphere of Mars: Effects of Electron Impact Ionization.

We use observations from the Mars Atmosphere and Volatile EvolutioN(MAVEN) mission to show how superthermal electron fluxes and crustal magnetic fields affect ion densities in the nightside ionosphere of Mars. We find that, due to electron impact ionization, high electron fluxes significantly increase the CO2+ , O+, and O2+ densities below 200 km, but only modestly increase the NO+ density. High electron fluxes also produce distinct peaks in the CO2+ , O+, and O2+ altitude profiles. We also find that superthermal electron fluxes are smaller near strong crustal magnetic fields. Consequently, nightside ion densities are also smaller near strong crustal fields because they decay without being replenished by electron impact ionization. Furthermore, the NO+/O2+ ratio is enhanced near strong crustal fields because, in the absence of electron impact ionization, O2+ is converted into NO+ and not replenished. Our results show that electron impact ionization is a significant source of CO2+ , O+, and O2+ in the nightside ionosphere of Mars.

Kinetics of microbial methionine metabolism in continuous cultures administered different methionine sources.

The Met precursor 2-hydroxy-4-(methylthio) butanoic acid (HMB) is expected to be more extensively degraded in the rumen than its isopropyl ester (HMBi). A control and 3 isomolar treatments-0.097% dl-methionine, 0.11% HMBi (HMBi), and 0.055% HMBi plus 0.048% Met (Met + HMBi)-were dosed every 8h simultaneously with 3-times-daily feeding into continuous cultures. Starting on d 9, for 6 consecutive doses, both [1-(13)C]-l-Met and [methyl-(2)H3]-l-Met replaced part of the unlabeled dl-Met, [(13)C5]-dl-HMBi replaced a portion of the unlabeled dl-HMBi, and [1-(13)C]-l-Met plus [(13)C5]-dl-HMBi replaced a portion of the respective unlabeled doses for the Met + HMBi treatment. After the sixth dose (d 11), unlabeled Met or HMBi provided 100% of the doses to follow elimination kinetics of the labels in HMBi, free Met, and bacterial Met compartments. The free [1-(13)C]-l-Met recycled more and was recovered in bacterial Met to a lesser extent than was the free [methyl-(2)H3]-l-Met recycling and that was recovered in bacterial Met. Increasing HMBi inclusion (0, 50, and 100% substitution of the exogenously dosed Met on a molar equivalent basis) tended to increase HMBi escape from 54.7 to 71.3% for the 50 and 100% HMBi treatments, respectively. Despite HMBi substituting for and decreasing the dosage of Met, increasing HMBi increased accumulation of free Met in fermenter fluid. The HMBi (after de-esterification of the isopropyl group) presumably produces Met through the intermediate α-ketomethylthyiobutyrate with an aminotransferase that also has high affinity for branched-chain AA. We provide evidence that the HMBi-derived Met is likely released from bacterial cells and accumulates rather than being degraded, potentially as a result of lagging d-stereoisomer metabolism. More research is needed to evaluate racemization and metabolism of stereoisomers of HMBi, Met, and other AA in ruminal microbes.

Assessing the ruminal action of the isopropyl ester of 2-hydroxy-4-(methylthio) butanoic acid in continuous and batch cultures of mixed ruminal microbes.

In dairy rations, Met is often a limiting amino acid that is provided by rumen-undegradable protein and rumen-protected sources of Met. A Met precursor, 2-hydroxy-4-(methylthio) butanoic acid (HMB) has undergone considerable study for ruminal and postruminal metabolism, whereas its isopropyl ester (HMBi) has been evaluated primarily with respect to its supply of metabolizable Met rather than as a preformed source of Met for microbial metabolism. A control and 3 isomolar Met treatments-0.097% dl-Met, 0.048% dl-Met plus 0.055% HMBi (Met + HMBi treatment), and 0.11% HMBi-were pulse-dosed every 8h into continuous cultures simultaneously with feeding. Treatment had no effect on digestibilities of acid-detergent fiber or true organic matter. Digestibilities of neutral detergent fiber and hemicellulose were linearly decreased with increasing HMBi inclusion. Concentration of NH3-N tended to decrease linearly and quadratically, and NH3-N flow tended to decrease linearly, with increasing HMBi inclusion; in contrast, the proportion of bacterial N derived from NH3-N increased linearly. Peptide N increased linearly and tended to be affected quadratically (highest for the HMBi treatment). Acetate and propionate production both decreased with increasing HMBi, but acetate declined more such that acetate:propionate increased linearly. Isobutyrate production decreased, but isovalerate and valerate increased with increasing HMBi inclusion. Relative changes in population abundance were not detected by denaturing gradient gel electrophoresis. In the second study, which was done in batch culture, Met treatments consisted of control, 0.097% l-Met, 0.097% l-Met, 0.125% dl-HMBi, 0.098% dl-HMB, 0.250% dl-HMBi (2× HMBi), 0.049% dl-Met + 0.063% dl-HMBi (Met + HMBi), and 0.098% dl-HMB + 0.039% isopropanol. All of these Met treatments were unlabeled (i.e., at natural abundance of (13)C) but simultaneously dosed with equivalent dosages of [1-(13)C]-l-Met. All 8 treatments were inoculated with faunated or partially defaunated inocula. Protozoal abundance had minor effect on measurements. The unlabeled l-Met treatment had the lowest (13)C enrichment of Met in the microbial pellet followed by Met + HMBi and then d-Met or dl-HMB, which were lower than remaining treatments. The percentage of the [1-(13)C]-l-Met dose recovered in microbial Met was lowest for the l-Met treatment; intermediate for d-Met, dl-HMB (with or without isopropanol), and Met + HMBi treatments; and highest for HMBi, 2× HMBi, and control. Results suggest that racemization of d-Met lags behind l-Met. The similar conversions of the HMBi and 2× HMBi treatments compared with the control suggests a low degradation of HMBi to provide unlabeled Met to dilute the [1-(13)C]-l-Met dose for protein synthesis. The lack of treatment by time interaction suggests that these initial responses carried through during the 24h of incubation. The proportion of HMBi available to ruminal microbes can influence microbial metabolism, potentially through formation of l-Met.

Carbon Ion Fluxes at Mars: First Results of Tailward Flows From MAVEN-STATIC.

Characterizing C+ ions in the Martian ionosphere is important for understanding the history of the Martian atmosphere and surface due to its place in understanding carbon escape. Measuring minor ions, like C+, which are close in mass to major atmospheric ions, in this case O+, is difficult, requiring fitting algorithms and accurate background subtraction. Accurate measurement of these species is essential for understanding chemistry and transport in the ionosphere. In this paper, we use data from the Mars Atmospheric and Volatile EvolutioN SupraThermal And Thermal Ion Composition (MAVEN-STATIC) sensor to report the first C+ fluxes measured in the Martian magnetotail. We will describe a multistep method of background subtraction as well as fitting routines that are used to extract C+ fluxes from a 40-orbit subset of STATIC data. Our results show tailward fluxes in both optical shadow and the adjacent sunlit magnetotail at high altitudes ( > 3,000 km) and Mars-ward at low altitudes ( < 2,000 km) in shadow. These local flux values are similar to estimates of neutral carbon fluxes from photochemical escape. However, total carbon loss comparisons will require a more comprehensive study of integrated C+ loss over a larger data set from the Martian magnetotail.

In Situ Measurements of Thermal Ion Temperature in the Martian Ionosphere.

In situ measurements of ionospheric and thermospheric temperatures are experimentally challenging because orbiting spacecraft typically travel supersonically with respect to the cold gas and plasma. We present O 2 + temperatures in Mars' ionosphere derived from data measured by the SupraThermal And Thermal Ion Composition instrument onboard the Mars Atmosphere and Volatile EvolutioN spacecraft. We focus on data obtained during nine special orbit maneuvers known as Deep Dips, during which MAVEN lowered its periapsis altitude from the nominal 150 to 120 km for 1 week in order to sample the ionospheric main peak and approach the homopause. We use two independent techniques to calculate ion temperatures from the measured energy and angular widths of the supersonic ram ion beam. After correcting for background and instrument response, we are able to measure ion temperatures as low as 100 K with associated uncertainties as low as 10%. It is theoretically expected that ion temperatures will converge to the neutral temperature at altitudes below the exobase region (∼180-200 km) due to strong collisional coupling; however, no evidence of the expected thermalization is observed. We have eliminated several possible explanations for the observed temperature difference between ions and neutrals, including Coulomb collisions with electrons, Joule heating, and heating caused by interactions with the spacecraft. The source of the energy maintaining the high ion temperatures remains unclear, suggesting that a fundamental piece of physics is missing from existing models of the Martian ionosphere.

Megagauss physics.

Fields greater than 10 MG can be produced by explosive flux compression and fields up to 3 MG with capacitor banks. Measurement of fields up to 10 MG is reliable, but difficulties may be expected at higher fields. Megagauss fields have been applied successfully as high-pressure sources, in high-energy particle physics, and in solid-state investigations. Other uses remain to be exploited: plasma compression by megagauss fields has been relatively unsuccessful but shows promise; their use as particle accelerators has been studied only theoretically; and much work remains to be done, both experimentally and theoretically, in connection with applications of megagauss fields in solidstate physics. Note added in proof: Since this article was prepared, Grigor'ev et al. have carried out some experiments (48) in which they have compressed hydrogen up to a density of 1.95 grams per cubic centimeter with a calculated pressure of 8 x 10(6) atmospheres. They report five different pressure-density points and claim that their data can be explained by assuming that the transition to the metallic phase occurs at a pressure of 2.8 x 10(6) atmospheres, with a density change from 1.08 to 1.3 g/cm(3). Using the flux compression techniques described earlier in this article, Hawke et al. [see (30, 31)] have obtained a pressure-density point at 1.5 x 10(6) atmospheres and 1.0 g/cm(3), which is also not inconsistent with a predicted equation of state of metallic hydrogen (49). In view of the experimental uncertainties, none of the pressure-density data can yet be used conclusively to establish the transition's existence. Hawke and his co-workers are presently engaged in measurements of the electrical conductivity of the compressed hydrogen. Observation of a significant conductivity at the proposed transition pressure would be a more definitive test of a metallic transition. In addition, two lower pressure-density points have been obtained for deuterium by the Los Alamos group, by means of the flux compression methods described earlier in this article. One point agrees to within experimental error with a slight extrapolation of Stewart's data (50). The second point is at a pressure of 65+/- 3 x 10(3) atmospheres with a density of 0.71 +/- 0.10 g/cm(3). The data are tentative, and efforts are under way to obtain more data points at both higher and lower pressures.

Polymorphism of shock loaded fe-mn and fe-ni alloys.

Addition of nickel or manganese to iron lowers the pressure of the "130-k" dynamic polymorphic transition to about 55 kilobars at the limits of the body-centered cubic alloy phase.

Marked long-term decline in ambient CO mixing ratio in SE England, 1997-2014: evidence of policy success in improving air quality.

Atmospheric CO at Egham in SE England has shown a marked and progressive decline since 1997, following adoption of strict controls on emissions. The Egham site is uniquely positioned to allow both assessment and comparison of 'clean Atlantic background' air and CO-enriched air downwind from the London conurbation. The decline is strongest (approximately 50 ppb per year) in the 1997-2003 period but continues post 2003. A 'local CO increment' can be identified as the residual after subtraction of contemporary background Atlantic CO mixing ratios from measured values at Egham. This increment, which is primarily from regional sources (during anticyclonic or northerly winds) or from the European continent (with easterly air mass origins), has significant seasonality, but overall has declined steadily since 1997. On many days of the year CO measured at Egham is now not far above Atlantic background levels measured at Mace Head (Ireland). The results are consistent with MOPITT satellite observations and 'bottom-up' inventory results. Comparison with urban and regional background CO mixing ratios in Hong Kong demonstrates the importance of regional, as opposed to local reduction of CO emission. The Egham record implies that controls on emissions subsequent to legislation have been extremely successful in the UK.

Dust observations at orbital altitudes surrounding Mars.

Dust is common close to the martian surface, but no known process can lift appreciable concentrations of particles to altitudes above ~150 kilometers. We present observations of dust at altitudes ranging from 150 to above 1000 kilometers by the Langmuir Probe and Wave instrument on the Mars Atmosphere and Volatile Evolution spacecraft. Based on its distribution, we interpret this dust to be interplanetary in origin. A comparison with laboratory measurements indicates that the dust grain size ranges from 1 to 12 micrometers, assuming a typical grain velocity of ~18 kilometers per second. These direct observations of dust entering the martian atmosphere improve our understanding of the sources, sinks, and transport of interplanetary dust throughout the inner solar system and the associated impacts on Mars's atmosphere.

Early MAVEN Deep Dip campaign reveals thermosphere and ionosphere variability.

The Mars Atmosphere and Volatile Evolution (MAVEN) mission, during the second of its Deep Dip campaigns, made comprehensive measurements of martian thermosphere and ionosphere composition, structure, and variability at altitudes down to ~130 kilometers in the subsolar region. This altitude range contains the diffusively separated upper atmosphere just above the well-mixed atmosphere, the layer of peak extreme ultraviolet heating and primary reservoir for atmospheric escape. In situ measurements of the upper atmosphere reveal previously unmeasured populations of neutral and charged particles, the homopause altitude at approximately 130 kilometers, and an unexpected level of variability both on an orbit-to-orbit basis and within individual orbits. These observations help constrain volatile escape processes controlled by thermosphere and ionosphere structure and variability.

MAVEN observations of the response of Mars to an interplanetary coronal mass ejection.

Coupling between the lower and upper atmosphere, combined with loss of gas from the upper atmosphere to space, likely contributed to the thin, cold, dry atmosphere of modern Mars. To help understand ongoing ion loss to space, the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft made comprehensive measurements of the Mars upper atmosphere, ionosphere, and interactions with the Sun and solar wind during an interplanetary coronal mass ejection impact in March 2015. Responses include changes in the bow shock and magnetosheath, formation of widespread diffuse aurora, and enhancement of pick-up ions. Observations and models both show an enhancement in escape rate of ions to space during the event. Ion loss during solar events early in Mars history may have been a major contributor to the long-term evolution of the Mars atmosphere.

Antiquity of the biological sulphur cycle: evidence from sulphur and carbon isotopes in 2700 million-year-old rocks of the Belingwe Belt, Zimbabwe.

Sulphur and carbon isotopic analyses on small samples of kerogens and sulphide minerals from biogenic and non-biogenic sediments of the 2.7 x 10(9) years(Ga)-old Belingwe Greenstone Belt (Zimbabwe) imply that a complex biological sulphur cycle was in operation. Sulphur isotopic compositions display a wider range of biological fractionation than hitherto reported from the Archaean. Carbon isotopic values in kerogen record fractionations characteristic of rubisco activity methanogenesis and methylotrophy and possibly anoxygenic photosynthesis. Carbon and sulphur isotopic fractionations have been interpreted in terms of metabolic processes in 2.7 Ga prokaryote mat communities, and indicate the operation of a diverse array of metabolic processes. The results are consistent with models of early molecular evolution derived from ribosomal RNA.

Cochlear implantation after labyrinthectomy.

OBJECTIVE: The goal was to report a method used for intraoperative ear selection for cochlear implantation using electrical brainstem response. Initial patient response and the longer-term results of cochlear implantation after labyrinthectomy were compared. STUDY DESIGN: This was a specific retrospective review of a single case of cochlear implantation after labyrinthectomy. SETTING: The study involved a tertiary referral center in both an ambulatory and a hospital setting. PATIENT: The study involved a report of a single patient who was evaluated for a possible cochlear implant and successfully underwent cochlear implantation. INTERVENTIONS: A case study of a profoundly deaf individual is presented, including the diagnostic measures used to determine the candidacy for cochlear implantation, the ear selected, and the rehabilitation. MAIN OUTCOME MEASURES: Both early (3 months) and later (14 months) postoperative results clearly demonstrate that a cochlear implant in a patient with a previous labyrinthectomy can be beneficial. RESULTS: The early and later results after cochlear implantation are compared in a single case study. CONCLUSION: This case study demonstrates that there is improvement in sound awareness, speech recognition, and communication after cochlear implantation in a previously labyrinthectomized ear.