The electron heating rate and ion chemistry in the thermosphere above Wallops Island during the solar eclipse of 7 March 1970

An identical pair of thermosphere probes measured the N2 concentration and temperature, the ion composition and concentrations and the electron temperature up to 290 km about 30 min and 5 min before totality during the 7 March 1970 eclipse at Wallops Island. The rockets travelled similar trajectories thus permitting the purely temporal changes between nights to be resolved. The neutral temperature and N2 concentration changed little but the electron temperature decreased by as much as 20 per cent in the lower F-region. The ion concentration decreased by about 30 per cent in the F-region and about 50 per cent in the E-region, with little change in relative ion composition. The electron cooling rates decreased by a factor of 6 in the lower F-region, approximately in proportion to the change in visible solar disc. A smaller than expected decrease in the cooling rate below 150 km between the two flights indicates a hardening of the solar spectrum and suggests a significant heat contribution from the solar corona near totality. The ion composition measurements were consistent with solutions of the ion continuity equations. A proper fit required a factor of three enhancement of the flux below 200 A, an amount also consistent with the electron heat balance analysis. Reactions involving the minor ions N+ and N2+ were found to be important for the ion chemistry of the major ions O2+ and NO+, especially at the time of eclipse. The negligible response of the neutral atmosphere to the eclipse is reasonable considering the long time constants for the conductive and convective transport processes and the local nature of the disturbance.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/34133/1/0000417.pd

Physiological and biochemical adaptations to training in Rana pipiens

Fifteen Rana pipiens were trained on a treadmill thrice weekly for 6.5 weeks to assess the effects of training on an animal that supports activity primarily through anaerobiosis. Endurance for activity increased 35% in these frogs as a result of training ( P =0.006, Fig. 1). This increased performance was not due to enhanced anaerobiosis. Total lactate produced during exercise did not differ significantly for the trained or untrained animals in either gastrocnemius muscle (2.77±0.21 and 2.82±0.13 mg/g, respectively) or whole body (1.32±0.10 and 1.47±0.06 mg/g, respectively). Glycogen depletion also did not differ between the two groups (Fig. 2c). The primary response to training appeared to involve augmentation of aerobic metabolism, a response similar to that reported for mammals. Gastrocnemius muscles of trained frogs underwent a 38% increase over those of untrained individuals in the maximum activity of citrate synthase (14.5±1.0 and 10.5±0.9 μmoles/(g wet wt·min); P =0.008). This enzyme was also positively correlated with the level of maximum performance for all animals tested ( r =0.61, P <0.01) and with the degree of improvement in the trained animals ( r =0.72, P <0.05). In addition to an increased aerobic capacity, the trained animals demonstrated a greater removal of lactate from the muscle 15 min after fatigue (Fig. 2b).Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/47124/1/360_2004_Article_BF00710002.pd

The poleward edge of the mid-latitude trough—its formation, orientation and dynamics

Data from the Advanced Ionospheric Sounder (AIS) deployed at Halley, Antarctica (76°S, 27°W; L = 4.2) and the Dynamics Explorer-2 spacecraft (DE-2) are used to investigate several aspects of the formation processes and dynamics of the poleward edge of the mid-latitude electron density trough. These include a study of the flux and energy of charged particles precipitating into the F-region as a function of Magnetic Local Time. It is found that local energetic electron precipitation is a major source of ionisation of the poleward edge in the evening sector, but after magnetic midnight transport processes become more important. Occasionally a significant increase in the flux of conjugate photo-electrons is co-located with the poleward edge of the trough in the morning sector. Some possible mechanisms are discussed but no firm conclusions are drawn. The combination of AIS and DE-2 data has allowed identification of significant longitudinal structure on the poleward edge of the trough that may be the result of substorm activity. It is found that the orientation of the poleward edge of the trough and the locus of the plasmapause predicted from the ‘tear-drop’ model vary in rather a similar manner with local time, though no close physical link between the two features is inferred from this coincidence. A comparison of the equatorward motion of the poleward edge on many nights is used to show that Kp is a poor index to use in any empirical model for predicting the temporal variations of the location of the trough. It is suggested that a more thorough understanding of the processes controlling the variability of the magnetospheric convection electric field is required before any significant improvement to the empirical models is likely to occur

The Very Deep Hole Concept: Evaluation of an Alternative for Nuclear Waste Disposal

One proposal for disposing of radioactive waste is to put it in drill holes or mined cavities so deep that the waste would be effectively isolated from the surface. Even if radioisotopes escaped from the disposal canister, they would be removed from the circulating groundwater system by sorption and/or chemical reaction in their transit on very long paths to the surface. This report summarizes the feasibilities and costs of making deep holes and deep mine shafts; estimates probable technological advances by the year 2000; presents thermal history and thermally induced stress calculations based on several assumptions regarding age of waste and density of emplacement; and summarizes lack of knowledge that bear upon the isolation of waste at great depth. In strong rock, present technology would probably enable us to drill a hole 20 cm in diameter to a depth of 11 km and sink a shaft 10 m in diameter to about 4.4 km. By the year 2000, with advancement of technology, holes of 15 km depth and 20 cm diameter could be drilled, and shafts of 6.4 km or deeper could be sunk. The heat output of 5.5-year-old spent fuel and 6.5-year-old reprocessed waste is used to calculate temperature increases and stress buildings in the surrounding rocks. Some waste configurations may cause unacceptably high temperature increases; indeed, limitations on temperatures reached will in some cases limit the packing density of waste canisters and/or require longer cooling of the waste before emplacement. Sealing boreholes and shafts for significant times, i.e. 1,000 to 100,000 years presents additional problems. The casing or ling of the borehole or shaft would have to be removed in the region where seals are constructed, or the lining material would have to be designed to function as an integral part of the long-term seal. Sealing fractures in the rock around the borehole or shaft will be quite important

The Mars Atmosphere and Volatile Evolution (MAVEN) Mission

The MAVEN spacecraft launched in November 2013, arrived at Mars in September 2014, and completed commissioning and began its one-Earth-year primary science mission in November 2014. The orbiter’s science objectives are to explore the interactions of the Sun and the solar wind with the Mars magnetosphere and upper atmosphere, to determine the structure of the upper atmosphere and ionosphere and the processes controlling it, to determine the escape rates from the upper atmosphere to space at the present epoch, and to measure properties that allow us to extrapolate these escape rates into the past to determine the total loss of atmospheric gas to space through time. These results will allow us to determine the importance of loss to space in changing the Mars climate and atmosphere through time, thereby providing important boundary conditions on the history of the habitability of Mars. The MAVEN spacecraft contains eight science instruments (with nine sensors) that measure the energy and particle input from the Sun into the Mars upper atmosphere, the response of the upper atmosphere to that input, and the resulting escape of gas to space. In addition, it contains an Electra relay that will allow it to relay commands and data between spacecraft on the surface and Earth