Identification and measurement of the combustible gases that occur in the gaseous metabolic products of sheep

This paper presents a review of the actual production, sales, and economic data from two production areas with 52 wells developed by a joint coal industry' gas industry effort owned equally by Jim Walter Resources, Inc. (JWR), a subsidiary of Jim Walter Corporation of Tampa, Florida and Enhanced Energy Resources, Inc. (EER), a subsidiary of Kaneb Services, Inc. of Houston, Texas. The unique reservoir characteristics of the coal environment are described in brief, a comparison of actual methane production from coal with computer model predictions is presented, and the capital and operating costs are discussed with specific emphasis on the economic results. This information differs from similar previous work in that economic vitality is now apparent whereas previous inquiries were essentially restricted to the technical reservoir engineering characteristics and the physical capability of coal to desorb (produce) methane. There are a number of published papers on this important technical aspect several of which are references for this presentation. Production Area I (31 well production area) has been generating an operating profit for the past 21 months. Profits have increased substantially in the past year as a result of the completion of an 8" transmission line and reduced operating costs. Initial production commenced in late 19/9. A five well pilot project was evaluated for approximately two years before commercial development commenced in late 1981. A total of 31 wells were drilled by mid-1982. First sales commenced in February of 1982. Production Area II drilling commenced in January of 1983 with initial sales in March of 1983. The economic viability is demonstrated based on actual operating profits over the past twenty-one months and current experience with respect to improvements in operational techniques and costs. These data are applied to the computer forecasts of long term dellverabilities for projections of expected economic performance.

Chapter 2 - Nitrogen, carbon dioxide, argon, neon, krypton, and xenon

Does the Moon's surface contain an archive of the early history of Earth? According to an intriguing idea, based on recently published analyses of lunar soils, it might do — and the proposal can be tested. The Moon as a whole is strongly depleted in volatile elements, but lunar soils contain large amounts of nitrogen and noble gases. The conventional explanation is that these elements derive from solar wind hitting the lunar surface. Now a decidedly unconventional suggestion has been made: what if nitrogen and noble gases originating on Earth also found their way to the Moon? The escape of atmospheric constituents is prevented today by the Earth's geomagnetic field. But the nitrogen isotope ratio in lunar soils cannot be explained by the accumulation of solar material alone: it is possible that substantial amounts of nitrogen and light noble gases could gave been transported from Earth's ancient atmosphere before the geomagnetic field developed. This proposal can be tested by comparing implanted materials in soils from near and far sides of the Moon. If a difference is found, another mystery might be solved: the age of Earth's geomagnetic field.

ABSTRACTPurpose: Few studies have directly compared excess postexercise oxygen consumption (EPOC) and fat utilization following different exercise intensities, and the effect of continuous exercise exceeding 75% of maximal oxygen uptake (VO2max) on these parameters remains unexplored. The current study examined EPOC and fat utilization following acute moderate- and vigorous-intensity continuous training (MICT and VICT) and sprint interval training (SIT). Methods: Eight active young men performed 4 experimental sessions: (a) MICT (30 min of running at 65% VO2max); (b) VICT (30 min of running at 85% VO2max); (c) SIT (4 30-s “all-out” sprints with 4 min of rest); and (d) no exercise (REST). Excess postexercise oxygen consumption and fat oxidation were estimated from gas measurements (VO2 and carbon dioxide production [VCO2]) obtained during a 2-hr postexercise period. Results: Total EPOC was similar (p = .097; effect size [ES] = 0.3) after VICT (8.6 ± 4.7 L) and SIT (10.0 ± 4.2 L) and greater after both (VICT, p = .025, ES = 0.3, and SIT, p < .001, ES = 0.6) versus MICT (6.0 ± 4.3 L). Fat utilization increased after MICT (0.047 ± 0.018 g· min−1, p = .018, ES = 1.3), VICT (0.066 ± 0.020 g•min−1, p = .034, ES = 2.2), and SIT (0.115 ± 0.026 g•min−1, p < .001, ES = 4.0) versus REST (0.025 ± 0.018 g•min−1) and was greatest after SIT (p < .001, ES = 3.0 vs. MICT; p = .031, ES = 2.1 vs. VICT). Conclusion: Acute exercise increases EPOC and fat utilization in an intensity-dependent manner.

The discovery of the helium rare gas in the wells in Saugor Division, southern Ganga Basin region has been done in Sagar District. The stable isotopic analyses were carried out for the gas samples collected from the 50 tube wells in Sagar and Damoh District of MP. The discovery of the rare gas helium in hydrocarbon rich zone in the tube wells in agricultural field at Garhakota, Rahatgarh, Bina, Banda and Sagar Tahsils, of District and Batiyagarh, Patharia, Jabera, tahsils in Damoh District of MP is a unique finding in rocks of the Vindhyan Super Group, in the history of Earth Science in India. The depth of tube wells varying from 300 to 750 ft. On the basis of geochemical analysis, it is remarkable to note that average values of helium contents varies from 0.34 to 0.732% along with the 72–99% of methane and ethane, and minor amount of oxygen, nitrogen, and CO2 gases in the hydrocarbon rich zone are recorded during the geochemical and stable isotope analysis. It has been found in the stable isotope δ C13 value, the values for the methane is −43.6 to −54.9‰ w.r.t. PDB. For the Ethane gas it is −24.9 to −26.4‰ w.r.t. PDB in the gas samples collected in the saturated sodium chloride solution in the glass bottles at various sites in Sagar and Damoh District. The occurrence of rare helium gas in the Hydrocarbon rich zone was reported for the first time in January, 2007 from the tube wells of Sagar District, which were geochemically and isotopically stable, analysed in the labs of KDMIPE Dehradun and NGRI Hydrabad. The gaseous hydrocarbon analysis shows the presence of moderate to low concentration of methane (C1) 1 to 104 ppb, Ethane (C2) −1 to 14 ppb, Propane (C3) 1 to 10 ppb, i-Butane (i C4) 1 to 9 ppb, and n Butane (n C4) 1 to 8 ppb in the soil samples collected from different locations. The result of the adsorbed soil gas and stable isotopic analysis of Ethane gas in these samples have δ C13 value ranging from −24.9‰ w.r.t. PDB and −26.9‰ w.r.t. PDB, and these are indicative that the gas is of thermogenic origin, which must have been formed at very high temperature and pressure condition in the deeper horizon of the Great Vindhyan sedimentary basin of an early Proterozoic (>600 m.y.) period.

This is an advance summary of a forthcoming article in the Oxford Encyclopedia of Planetary Science. Please check back later for the full article.Although the second most abundant element in the cosmos is helium, noble gases are also called rare gases. The reason is that they are not abundant on terrestrial planets like our Earth, which is characterized by orders of magnitude depletion of—particularly light—noble gases when compared to the cosmic element abundance pattern. Indeed, such geochemical depletion and enrichment processes make noble gases so versatile concerning planetary formation and evolution: When our solar system formed, the first small grains started to adsorb small amounts of noble gases from the protosolar nebula, resulting in depletion of light He and Ne when compared to heavy noble gases Ar, Kr, and Xe: the so-called planetary type abundance pattern. Subsequent flash heating of the first small mm to cm-sized objects (chondrules and calcium, aluminum rich inclusions) resulted in further depletion, as well as heating—and occasionally differentiation—on small planetesimals, which were precursors of larger planets and which we still find in the asteroid belt today from where we get rocky fragments in form of meteorites. In most primitive meteorites, we even can find tiny rare grains that are older than our solar system and condensed billions of years ago in circumstellar atmospheres of, for example, red giant stars. These grains are characterized by nucleosynthetic anomalies and particularly identified by noble gases, for example, so-called s-process xenon.While planetesimals acquired a depleted noble gas component strongly fractionated in favor of heavy noble gases, the sun and also gas giants like Jupiter attracted a much larger amount of gas from the protosolar nebula by gravitational capture. This resulted in a cosmic or “solar type” abundance pattern, containing the full complement of light noble gases. Contrary to Jupiter or the sun, terrestrial planets accreted from planetesimals with only minor contributions from the protosolar nebula, which explains their high degree of depletion and basically “planetary” elemental abundance pattern. Indeed this depletion enables another tool to be applied in noble gas geo- and cosmochemistry: ingrowth of radiogenic nuclides. Due to heavy depletion of primordial nuclides like 36Ar and 130Xe, radiogenic ingrowth of 40Ar by 40K decay, 129Xe by 129I decay, or fission Xe from 238U or 244Pu decay are precisely measurable, and allow insight in the chronology of fractionation of lithophile parent nuclides and atmophile noble gas daughters, mainly caused by mantle degassing and formation of the atmosphere.Already the dominance of 40Ar in the terrestrial atmosphere allowed C. F v. Weizsäcker to conclude that most of the terrestrial atmosphere originated by degassing of the solid Earth, which is an ongoing process today at mid ocean ridges, where primordial helium leaves the lithosphere for the first time. Mantle degassing was much more massive in the past; in fact, most of the terrestrial atmosphere formed during the first 100 million years of Earth´s history, and was completed at about the same time when the terrestrial core formed and accretion was terminated by a giant impact that also formed our moon. However, before that time, somehow also tiny amounts of solar noble gases managed to find their way into the mantle, presumably by solar wind irradiation of small planetesimals or dust accreting to Earth. While the moon-forming impact likely dissipated the primordial atmosphere, today´s atmosphere originated by mantle degassing and a late veneer with asteroidal and possibly cometary contributions. As other atmophile elements behave similar to noble gases, they also trace the origin of major volatiles on Earth, for example, water, nitrogen, sulfur, and carbon.

The mechanisms of carbon dioxide flooding at pressures below the minimum miscibility pressure (MMP) were studied using a numerical model of a slim tube to determine a means of increasing the efficiency of such floods. Results of these studies indicate that, in multiple contact flooding (MCF), the gas phase at the liquid-gas front approaches a constant composition denoting a bank of solvent approaching conditions of miscibility, but not achieving it because of the quantity of methane, nitrogen, and other light gases that overwhelms it. The ethane plus components (C2+) composed approximately five percent of the reservoir gas phase. This constant compositional gas phase formed early in the flood and persisted throughout the flood until eventual gas breakthrough. A simulated low-temperature flash of the reservoir gas phase produced a solvent that contained more than 75 percent ethane and propane. Slugs of this solvent were used to produce miscible displacements with CO2 gas at pressures 40 percent below the MMP. These findings were confirmed in further studies using fluids from several other reservoirs.

The evolution of terrestrial volatiles: a view from helium, neon, argon and nitrogen isotope modelling

Anaerobic digestion is a microorganism-mediated redox system which is chemically represented by Buswell&amp;rsquo;s equation. In the equation, quantity of methane and carbon dioxide can be counted by the elemental composition of organic matter, however there is a lack of connection between electron transfer and formations of methane and carbon dioxide. Although the mechanism of direct interspecies and mediated interspecies electron transfer in anaerobic digestion has been widely researched, the method of counting electron transfer in Buswell&amp;rsquo;s equation has not yet been explored. This article develops a method to count electron transfer of organic molecules in Buswell&amp;rsquo;s equation. Mathematical equations are established through integration of relationships among mean oxidation number of organic carbons, quantity of methane, and number of transferred electrons. With any known organic structural formula, three tasks can be achieved: (1) determine the Buswell-Ratio, (2) count Buswell-Electron, and (3) demonstrate electron transfer among organic carbons by drawing the Buswell-Electron diagram.

Formation of carbon oxides during tobacco combustion: Pyrolysis studies in the presence of isotopic gases to elucidate reaction sequence

The syngas production performance of scrap iron reacting with carbon dioxide and water steam was assessed under different operating conditions in a fixed bed oxidizer reactor. The syngas generation step is part of a novel process scheme encompassing the reutilization of iron scrap from steelmaking and the combined splitting of industrially captured carbon dioxide and steam into a syngas. At 1050 °C, a maximum volume percentage of 37 % carbon monoxide was detected in the product gas with the injection of 1 NL/min carbon dioxide. The carbon dioxide conversion was confirmed to be promoted by temperature. Subsequently, combined tests with carbon dioxide and water steam were carried out to assess the production and quality of the syngas (H2 and CO) by varying the reactants total flow rate, the iron bed mass and the reactants molar ratio. By decreasing the total reactants flow rate, the reactants splitting process was promoted and below a certain flow rate carbon dioxide splitting prevailed on that of water steam. By increasing the H2Ov/CO2 molar ratio, the splitting was enhanced for both species. In particular, for the tested flow rate the water splitting increased by 10% compared to 3.5% of the CO2 splitting. This indicated that a high H2Ov/CO2 ratio optimizes syngas production in the designed system. Finally, with H2Ov/CO2 = 6 and the optimal thermochemical syngas composition was achieved, including 41 % H2 and 12.1 % CO, being the remaining part constituted by CO2 when computed on a dry basis.

Noble gases are exceptional tracers in continental settings due to the remarkable isotopic variability between the mantle, crust, and atmosphere, and because they are inert. Due to systematic variability in physical properties, such as diffusion, solubility, and production rates, the combination of helium, neon, and argon provides unique but under-utilized indices of gas migration. Existing noble gas data sets are dominated by measurements of gas and fluid phases from gas wells, ground waters and hot springs. There are very few noble gas measurements from the solid continental crust itself, which means that this important reservoir is poorly characterized. The central goal of this project was to enhance understanding of gas distribution and migration in the continental crust using new measurements of noble gases in whole rocks and minerals from existing continental drill cores, with an emphasis on helium, neon, argon. We carried out whole-rock and mineral-separate noble gas measurements on Precambrian basement samples from the Texas Panhandle. The Texas Panhandle gas field is the southern limb of the giant Hugoton-Panhandle oil and gas field; it has high helium contents (up to ~ 2 %) and 3He/4He of 0.21 (± 0.03) Ra. Because the total amount of helium in the Panhandle gas field is relatively well known, crustal isotopic data and mass balance calculations can be used to constrain the ultimate source rocks, and hence the helium migration paths. The new 3He/4He data range from 0.03 to 0.11 Ra (total), all of which are lower than the gas field values. There is internal isotopic heterogeneity in helium, neon, and argon, within all the samples; crushing extractions yield less radiogenic values than melting, demonstrating that fluid inclusions preserve less radiogenic gases. The new data suggest that the Precambrian basement has lost significant amounts of helium, and shows the importance of measuring helium with neon and argon. The 4He/40Ar values are particularly useful in demonstrating helium loss because all the data falls well below the production ratio.

Although the second most abundant element in the cosmos is helium, noble gases are also called rare gases. The reason is that they are not abundant on terrestrial planets like the Earth, which is characterized by orders of magnitude depletion of—particularly light—noble gases when compared to the cosmic element abundance pattern. Indeed, geochemical depletion and enrichment processes mean that noble gases are highly versatile tracers of planetary formation and evolution. When our solar system formed—or even before—small grains and first condensates incorporated small amounts of noble gases from the surrounding gas of solar composition, resulting in depletion of light He and Ne relative to heavy Ar, Kr, and Xe, leading to the “planetary type” abundance pattern. Further noble gas depletion occurred during flash heating of mm- to cm-sized objects (chondrules and calcium, aluminum-rich inclusions), and subsequently during heating—and occasionally differentiation—on small planetesimals, which were precursors of planets. Some of these objects are present today in the asteroid belt and are the source of many meteorites. Many primitive meteorites contain very small (micron to sub-micron size) rare grains that are older than our Solar System and condensed billions of years ago in in the atmospheres of different stars, for example, Red Giant stars. These grains are characterized by nucleosynthetic anomalies, in particular the noble gases, such as so-called s-process xenon. While planetesimals acquired a depleted noble gas component strongly fractionated in favor of heavy noble gases, the Sun and also gas giants like Jupiter attracted a much larger amount of gas from the protosolar nebula by gravitational capture. This resulted in a cosmic or “solar type” abundance pattern, containing the full complement of light noble gases. In contrast, terrestrial planets accreted from planetesimals with only minor contributions from the gaseous component of the protosolar nebula, which accounts for their high degree of depletion and essentially “planetary” elemental abundance pattern. The strong depletion in noble gases facilitates their application as noble gas geo- and cosmochronometers; chronological applications are based on being able to determine noble gas isotopes formed by radioactive decay processes, for example, 40Ar by 40K decay, 129Xe by 129I decay, or fission Xe from 238U or 244Pu decay. Particularly ingrowth of radiogenic xenon is only possible due to the depletion of primordial nuclides, which allows insight into the chronology of fractionation of lithophile parent nuclides and atmophile noble gas daughters. Applied to large-scale planetary reservoirs, this helps to elucidate the timing of mantle degassing and evolution of planetary atmospheres. Applied to individual rocks and minerals, it allows radioisotope chronology using short-lived (e.g., 129I–129Xe) or long-lived (e.g., 40K–40Ar) systems. The dominance of 40Ar in the terrestrial atmosphere allowed von Weizsäcker to conclude that most of the terrestrial atmosphere originated by degassing of the solid Earth, which is an ongoing process today at mid-ocean ridges, as indicated by outgassing of primordial helium from newly forming ocean crust. Mantle degassing was much more massive in the past, with most of the terrestrial atmosphere probably formed during the first few 100 million years of Earth’s history, in response to major evolutionary processes of accretion, terrestrial core formation, and the terminal accretion stage of a giant impact that formed our Moon. During accretion, solar noble gases were added to the mantle, presumably by solar wind irradiation of the small planetesimals and dust accreting to form the Earth. While the Moon-forming impact likely dissipated a major fraction of the primordial atmosphere, today’s atmosphere originated by addition of a late veneer of asteroidal and possibly cometary material combined with a decreasing rate of mantle degassing over time. As other atmophile elements behave similarly to noble gases, they also trace the origin of major volatiles on Earth, for example, water, nitrogen, and carbon.

NEREUS/ Kemonaut, a mobile autonomous underwater mass spectrometer

Background and objective: The paper aims to estimate the environmental gases of Landfill No. 2 in Shahin Shahr (total landfill gas, methane gas and carbon dioxide gas), comparison of gas emissions over a period of 30 years, and the availability of landfill for energy extraction. Methods: The field of research is Landfill No. 2 at Shahin Shahr Recycling Plant (Isfahan) located in Jarfarabad Mountains, whose capacity was completed in 1391 and landfill gas assessment was carried out. The total amount of produced gases, methane and carbon dioxide has been calculated using the first-order degradation model over a period of 30 years. Results: The amount of these gases in Landfill has been calculated from 1394 to 1424.The results show that the amount of landfill gases has declined over time. The most amounts of methane and carbon dioxide production is about 1050000 and 287000 kilograms in 1394 and the least amount of methane and carbon dioxide production is estimated about 174 and 476 thousand kilograms, respectively, in 1424. The total volume of gases produced in this landfill has been estimated to be about 15 million cubic meters in 30 years, of which 27 percent are methane and 73 percent are carbon dioxide. The amount of methane and carbon dioxide gas is estimated to be about 15 million and 42 million kilograms in 30 years, respectively. Conclusion: Generally, landfill gases have declined over time. It is recommended to use energy recovery technologies for controlling greenhouse gas emissions and generation of required energy for the ShahinShahr recycling plant in order to use this volume of gas. n