D/H ratios of the inner Solar System

The original hydrogen isotope (D/H) ratios of different planetary bodies may indicate where each body formed in the Solar System. However, geological and atmospheric processes can alter these ratios through time. Over the past few decades, D/H ratios in meteorites from Vesta and Mars, as well as from S- and C-type asteroids, have been measured. The aim of this article is to bring together all previously published data from these bodies, as well as the Earth, in order to determine the original D/H ratio for each of these inner Solar System planetary bodies. Once all secondary processes have been stripped away, the inner Solar System appears to be relatively homogeneous in terms of water D/H, with the original water D/H ratios of Vesta, Mars, the Earth, and S- and C-type asteroids all falling between δD values of −100‰ and −590‰. This homogeneity is in accord with the ‘Grand tack’ model of Solar System formation, where giant planet migration causes the S- and C-type asteroids to be mixed within 1 AU to eventually form the terrestrial planets

Customer Acceptance is the Key to Success of Electronic Bill Presentment and Payment

This thesis focuses on issue of broaden Customer Acceptance in Electronic Bill Presentation andPayment (EBPP). Following the overview of EBPP’s concept, benefit, snapshot of the overall marketplace, the thesis studies the current existing models with it’s entity, process, and relationship. The important part of the thesis is to explore the main elements to one of the key barriers of EBPP, Customer acceptance according to TAM (Technology Acceptance Model) and Diffusion of Innovation Model, and provides the several key solutions to broaden Customer acceptance of EBPP. The thesis concludes with pointing out the limitation of this thesis and the suggestion of possible future research and looking forward to the future market of EBPP. Thesis contains five chapters. The CHAPTER I. INTRODUCTION defines the EBPP is the delivery of bills from Billers to Customers mainly through Internet; reviews the benefits to the both Biller and Customer; realizes the EBPP’s potential market growth with current low’adoption rate tepid the EBPP deployment. The CHAPTER II. ENTITY, PROCESS, AND RELATIONSHIP OF EBPP MODELS studies the six entities of EBPP, included Biller, Biller Service Provider, Biller Payment Provider, Customer, Customer Service Provider, Customer Payment Provider, and process of EBPP with Service Initiation, Bill Presentment, and Payment and Remittance. The complex process with a range of models, which include direct, consolidator, and syndicator is discussed. CHAPTER III. EXPLORE THE ELEMENTS TO AFFECT CUSTOMER ACCEPTANCE TO DEPLOY EBPP points out that low Customer acceptance impedes EBPP growth, studies the EBPP literature and user acceptance model in MIS, and explores the four factors (usefulness, ease of use, observability, and risk) and related elements affect the Customer acceptance, which are Customer low awareness, lack of a compelling reason, lack of incentive, trust and risk, uncertainty about security and privacy, inaccuracy and unreliable, difficult to use, bank slow react, legal issue, standard, and poor Customer service. CHAPTER IV. SOLUTION ANDSTRATEGY TO BROADEN CUSTOMER ACCEPTANCE OF EBPP suggests six solutions to broaden the Customer acceptance, which are chose right model, build solid EBPP system, chose a right vendor, and provide good Customer service, make aggressive marketing approach, and be proactive bank and Biller. CHAPTER V. CONCLUSION provides the overall of future market of EBPP

The origin of alteration “orangettes” in Dhofar 019: Implications for the age and aqueous history of the shergottites

The shergottites are the largest group of Martian meteorites, and the only group that has not been found to contain definitive evidence of Martian aqueous alteration. Given recent reports of current liquid water at the surface of Mars, this study aimed to investigate in detail the possibility of Martian phyllosilicate within shergottite Dhofar 019. Optical and scanning electron microscopy, followed by transmission electron microscopy, confirmed the presence of alteration orangettes, with a layered structure consisting of poorly ordered Mg-phyllosilicate and calcite. These investigations identified maskelynite dissolution, followed by Mg-phyllosilicate and calcite deposition within the dissolution pits, as the method of orangette production. The presence of celestine within the orangette layers, the absence of shock dislocation features within calcite, and the Mg-rich nature of the phyllosilicate, all indicate a terrestrial origin for these features on Dhofar 019

Formation of iddingsite veins in the martian crust by centripetal replacement of olivine: evidence from the nakhlite meteorite Lafayette

The Lafayette meteorite is an olivine clinopyroxenite that crystallized on Mars ∼1300 million years ago within a lava flow or shallow sill. Liquid water entered this igneous rock ∼700 million years later to produce a suite of secondary minerals, collectively called ‘iddingsite’, that occur as veins within grains of augite and olivine. The deuterium/hydrogen ratio of water within these secondary minerals shows that the aqueous solutions were sourced from one or more near-surface reservoirs. Several petrographically distinct types of veins can be recognised by differences in their width, shape, and crystallographic orientation. Augite and olivine both contain veins of a very fine grained hydrous Fe- and Mg-rich silicate that are ∼1-2 micrometres in width and lack any preferred crystallographic orientation. These narrow veins formed by cementation of pore spaces that had been opened by fracturing and probably in response to shock. The subset of olivine-hosted veins whose axes lie parallel to (001) have serrated walls, and formed by widening of the narrow veins by interface coupled dissolution-precipitation. Widening started by replacement of the walls of the narrow precursor veins by Fe-Mg silicate, and a crystallographic control on the trajectory of the dissolution-precipitation front created micrometre-scale {111} serrations. The walls of many of the finely serrated veins were subsequently replaced by siderite, and the solutions responsible for carbonation of olivine also partially recrystallized the Fe-Mg silicate. Smectite was the last mineral to form and grew by replacement of siderite. This mineralization sequence shows that Lafayette was exposed to two discrete pulses of aqueous solutions, the first of which formed the Fe-Mg silicate, and the second mediated replacement of vein walls by siderite and smectite. The similarity in size, shape and crystallographic orientation of iddingsite veins in the Lafayette meteorite and in terrestrial basalts demonstrates a common microstructural control on water-mineral interaction between Mars and Earth, and indicates that prior shock deformation was not a prerequisite for aqueous alteration of the martian crust

Think critically: evaluate that information!

Come examine how adding critical thinking components can meaningfully introduce the resources and services available through the library. Designing assignments with critical thinking components changes the focus from locating a thing to thinking about the relationship between things; between the topic and the key words that describe the idea; between the OPAC and the items on the shelf; between discovery and the quality of information. Examples will demonstrate how assignments emphasizing process and resourcefulness engage students to think through the search process and highlight the link between assignments and the various locations, services and resources needed

Library Assignments Beyond the Essay

Rather than bringing students to the library, bring library resources to you’re students through using critical thinking skills in a managing information exercise that uses locating and evaluating information to emphasize concepts within your class. Examples will include broader context for designing library instruction that echoes the courses’ content

Discovery Services: An Academically Enhanced Google?

Google prepared all of us for a single-search box window to access resources, and libraries recently adopted discovery services to accommodate this expectation. This service collates resources into a single-box search environment, and permits users to filter the results into meaningful groups that reinforce the research process. Teaching students to “think” their way through the search-process facilitates critical thinking skills

The Geology of the Moon: Geochemistry and Petrology of Lunar Basalts

The aim of this research is to determine any genetic relationships between high- and lowTi lunar basalts in terms of petrology, mineralogy, geochemistry and geochronology, using a set of Apollo samples. SEM images, mineral compositions, and major- and trace-element data indicate that the high and low-Ti mare-basalts form two distinct groups, both mineralogically and chemically. Apollo 12 and 15 low-Ti basalts were produced from similar source regions, whereas the Apollo 11 and 17 basalts show greater source region compositional variation. Pb-Pb age dating of low-Ti and high-Ti samples confirm previous observations indicating the former are generally younger than the latter. Geochemical modelling suggests that the low-Ti basalts formed from < 10 % partial melting of a depleted Moon source, followed by olivine fractionation. The high-Ti basalts were probably formed as a result of < 15 % partial melting of relatively incompatible-elementenriched source regions, followed by multi-phase crystal fractionation. The REE content of Apollo 14 low-Ti, high-AI basalt 14053 can be reconstructed by ~ 10 % partial melting of a depleted Moon source, followed by olivine fractionation and 1.5 % simultaneous assimilation of a KREEPy/granitic crustal component. The REE contents of Apollo 11 high-Ti, high-K basalts match well with 10 % KREEP assimilation, along with multi-phase fractionation from a parental melt similar to Apollo 11 orange glass. Setting aside the different parental melt evolutions, bulk-rock elemental evidence clearly indicates that the high- and low-Ti mare-basalts were produced by compositionally different source regions. This conclusion is supported by different oxygen isotope compositions of the high- and low-Ti basalts. However, oxygen isotope data implies that rather than a bi-modal system, a mare-basalt compositional continuum exists. This continuum fits well with the heterogeneous cumulate source model for mare-basalt formation. Our oxygen isotope data reveal no detectable difference between the 0 of the Earth and Moon, with implications for the viability of the giant impact origin of the Moon

The Geology of the Moon: Geochemistry and Petrology of Lunar Basalts

The aim of this research is to determine any genetic relationships between high- and lowTi lunar basalts in terms of petrology, mineralogy, geochemistry and geochronology, using a set of Apollo samples. SEM images, mineral compositions, and major- and trace-element data indicate that the high and low-Ti mare-basalts form two distinct groups, both mineralogically and chemically. Apollo 12 and 15 low-Ti basalts were produced from similar source regions, whereas the Apollo 11 and 17 basalts show greater source region compositional variation. Pb-Pb age dating of low-Ti and high-Ti samples confirm previous observations indicating the former are generally younger than the latter. Geochemical modelling suggests that the low-Ti basalts formed from < 10 % partial melting of a depleted Moon source, followed by olivine fractionation. The high-Ti basalts were probably formed as a result of < 15 % partial melting of relatively incompatible-elementenriched source regions, followed by multi-phase crystal fractionation. The REE content of Apollo 14 low-Ti, high-AI basalt 14053 can be reconstructed by ~ 10 % partial melting of a depleted Moon source, followed by olivine fractionation and 1.5 % simultaneous assimilation of a KREEPy/granitic crustal component. The REE contents of Apollo 11 high-Ti, high-K basalts match well with 10 % KREEP assimilation, along with multi-phase fractionation from a parental melt similar to Apollo 11 orange glass. Setting aside the different parental melt evolutions, bulk-rock elemental evidence clearly indicates that the high- and low-Ti mare-basalts were produced by compositionally different source regions. This conclusion is supported by different oxygen isotope compositions of the high- and low-Ti basalts. However, oxygen isotope data implies that rather than a bi-modal system, a mare-basalt compositional continuum exists. This continuum fits well with the heterogeneous cumulate source model for mare-basalt formation. Our oxygen isotope data reveal no detectable difference between the 0 of the Earth and Moon, with implications for the viability of the giant impact origin of the Moon

Compositional analysis of the very-low-Ti mare basalt component of NWA 773 and comparison with low-Ti basalts, LAP03632 and LAP02436

Abstract not available