On conjectures of Foulkes, Siemons and Wagner and Stanley

Let A = (AI, ... ,Ar ) be a partition of n. An unordered A-tabloid is a partition of the set {I, 2, ... , n} into r pairwise disjoint sets of sizes AI, ,Ar . Let F denote the field of complex numbers and C the symmetric group of {I, 2, , n}. Define HA to be the permutation module of FC whose basis is the set of unordered A-tabloids. Foulkes conjectured in [13] that there exists an injective FC-homomorphism H(b a ) -t H(a b ) when a ::; b. Independently Siemons and Wagner [27] and Stanley [29] generalized this conjecture to ask if there exists an injective map HA -t HA'. In this thesis we investigate these conjectures.EThOS - Electronic Theses Online ServiceGBUnited Kingdo

An interactive job seeking system for vocational rehabilitation

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Developing through mentoring or being mentored: ALDinHE’s new mentoring scheme and certified mentor recognition

ALDinHE is launching its new mentoring scheme and mentorship recognition to acknowledge, promote and recognise the importance of mentoring for learning development as a field that does not offer an official route into the profession. This Professional Development session introduced the mentoring scheme, explaining how to get involved, what support mentors and mentees can receive from ALDinHE and what benefits both sides can get from mentoring or being mentored. If you’re new to learning development or keen to develop more experience in a specific area with the help of a mentor, the mentoring scheme will offer you a brilliant framework to broaden your expertise. If you’re an experienced learning developer or have specific expertise you could share, find out how you could become recognised as a Certified Mentor (CeM) in learning development by ALDinHE

Mentoring in learning development

Learning Development is still a relatively young field (Syska and Buckley, 2022), and despite a growing body of research, it remains strongly practice-oriented. This means that experience, in this case of individual Learning Developers, takes an even more central place than it does in more established fields, and sharing this experience through mentoring takes on a central role. This is why the mentoring working group has developed a Learning Development focused ALDinHE Mentoring Scheme, together with a Certified Mentor recognition that helps experienced mentors be recognised for their contribution to growing and sharing LD knowledge. This mini keynote briefly introduced the Mentoring Scheme and the CeM recognition before exploring the role mentoring can play in the professional development of Learning Developers with the audience. The questions we asked were: What benefits would you expect for mentees? What benefits would you expect for mentors? What kind of experience can be best shared through mentoring

Development of Life on Early Mars

Exploration of Mars has begun to unveil the history of the planet. Combinations of remote sensing, in situ compositional measurements and photographic observations have shown Mars had a dynamic and active geologic evolution. Mars geologic evolution encompassed conditions that were suitable for supporting life. A habitable planet must have water, carbon and energy sources along with a dynamic geologic past. Mars meets all of these requirements. The first 600 My of Martian history were ripe for life to develop because of the abundance of (i) Water- as shown by carved canyons and oceans or lakes with the early presence of near surface water shown by precipitated carbonates in ALH84001, well-dated at ~3.9 Gy, (ii) Energy from the original accretional processes, a molten core which generated a strong magnetic field leaving a permanent record in the early crust, active volcanism continuing throughout Martian history, and continuing impact processes, (iii) Carbon, water and a likely thicker atmosphere from extensive volcanic outgassing (i.e. H20, CO2, CH4, CO, O2, N2, H2S, SO2, etc.) and (iv) crustal tectonics as revealed by faulting and possible plate movement reflected by the magnetic pattern in the crust [1]. The question arises: "Why would life not develop from these favorable conditions on Mars in its first 600 My?" During this period, environmental near-surface conditions on Mars were more favorable to life than at any later time. Standing bodies of water, precipitation and flowing surface water, and possibly abundant hydrothermal energy would favor the formation of early life. (Even if life developed elsewhere on Earth, Venus, or on other bodies-it was transported to Mars where surface conditions were suitable for life to evolve). The commonly stated requirement that life would need hundreds of millions of year to get started is only an assumption; we know of no evidence that requires such a long interval for the development of life, if the proper habitable conditions are meet. Perhaps it could start in a very short interval during the first tens of millions of years after crustal formation. Even with impact-driven extinction events, such a short start-up time would allow life to restart multiple times until it persevered. If panspermia is considered, life could be introduced as soon as liquid surface water was present and could instantly thrive and spread

Observation and analysis of in situ carbonaceous matter in Nakhla: Part I

New analyses of indigenous secondary material in the martian meteorite Nakhla reveal amorphous carbon-rich veins and dendrites. The texture and chemistry of this material resembles that of biogenically altered sub-ocean basaltic glasses

FE-SEM, FIB and TEM Study of Surface Deposits of Apollo 15 Green Glass Volcanic Spherules

Surface deposits on lunar pyroclastic green (Apollo 15) and orange (Apollo 17) glass spherules have been attributed to condensation from the gas clouds that accompanied fire-fountain eruptions. The fire fountains cast molten lava high above the lunar surface and the silicate melt droplets quenched before landing producing the glass beads. Early investigations showed that these deposits are rich in sulfur and zinc. The deposits are extremely fine-grained and thin, so that it was never possible to determine their chemical compositions cleanly by SEM/EDX or electron probe x-ray analysis because most of the excited volume was in the under-lying silicate glass. We are investigating the surface deposits by TEM, using focused ion beam (FIB) microscopy to extract and thin the surface deposits. Here we report on chemical mapping of a FIB section of surface deposits of an Apollo green glass bead 15401using the ultra-high resolution JEOL 2500 STEM located at NASA Johnson Space Center

Observation and analysis of in situ carbonaceous matter in Nakhla: part II

Analysis of in situ carbonaceous matter in the Nakhla SNC meteorite has been carried out using a variety of techniques. Laser raman data shows the carbonaceous matter to be highly complex and static mass spectrometry has shown it to have an isotopic composition of '18 to '20' C

Volcanic Coatings on Picritic Apollo 17 Glasses; Submicrometer-Deposits of Fe-CR-Metal

The purposes of our ongoing investigations of Apollo 15 green and Apollo 17 orange and black volcanic glasses are threefold: first, to increase our understanding of the volcanic origin of the glasses; second, to determine the nature of the coating materials deposited on the glasses during their cooling in the volcanic environment; and, third, to help determine the nature of the gases involved in the volcanic fire-fountaining that occurred at approximately 3.5 Ga on the moon. We are continuing studies of coatings on volcanic glasses using analytical techniques not available when these glasses were originally studied; these include high-resolution FE-TEM and X-ray mapping, along with other highly detailed methods including TEM electron diffraction analysis. Initial studies of Apollo 15 green volcanic glasses using the techniques described above revealed for the first time the presence of areas containing distinct layering of volcanic surface deposits. S was associated with some of the inner layer of metallic Fe but was absent from the outer layer. Zn was associated with S in some places in the inner layer. An example of a typical spherule used for this study is shown in Fig. 1. It is a black (quench-crystallized) bead from near the bottom of the 74001/2 double drive tube; black beads such as this one are essentially identical in composition to the orange (uncrystallized) beads of the 74001/2 core