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A trinitarian theological anthropology of male-female difference
Get PDFIn this thesis, I draw from trinitarian theology and Christology to develop an anthropological model of male-female relations. I argue that human male-female difference and the male-female relation (defined as relations between biologically male and biologically female humans) offer a unique set of insights for understanding personal relations more generally, and apply learnings from recent developments in theology to improve treatments of this topic in theological anthropology. I first draw from theories of the ontology of relations to explain how the Trinity exemplifies personal relations that are non-symmetrical but do not imply or require ontological priority of one person over another (expressed crudely: we can say that males and females are equal but different, using a rationale that has parallels with the argument that Father, Son and Spirit are equal but different). I argue that inner trinitarian relations can be used to understand male-female relations by using the imago dei concept and examining the personhood of Jesus Christ, who is the image of God in which all humans (male and female) are created. I review the historical development of theological treatments of the imago dei and Christology as they pertain directly to characterizing male-female relations, identifying and critiquing thinkers whose work highlights key questions in the debate. Then, using historical and modern Christology, I move to the theological anthropology of relations, defending the idea that male-female difference in humans is the paradigmatic form of personal differentiation in the created order and identifying ways that recent trinitarian theology and Christology can improve the characterization of male-female relations. Finally, I use the resulting relational model to draw conclusions about key questions in the history of the topic of male-female difference
From the Mythic to the Manègethe horse as intermediary between classical and Renaissance poetry in the work of Ronsard
Get PDFRonsard’s passion for the equestrian arts and his technical knowledge of the practice can be felt throughout his poetry. A contemporary at the royal stables of the riding master François de Carnavalet, the poet fuses his personal equestrian experiences from that time to the classical stories of horses of the past in order to praise at once the art of horsemanship and the art of poetry.Peer reviewe
2-fluorobenzyl (Z)-2-(5-chloro-2-oxoindolin-3-ylidene)hydrazine-1-carbodithioate dimethyl sulfoxide monosolvate
Get PDFFunding: The authors acknowledge Universiti Teknologi MARA for financial support.In the title solvate, C16H11ClFN3OS2·C2H6OS, the C=N bond adopts a Z-configuration facilitating the formation of an intramolecular N—H⋯O hydrogen bond to the carbonyl O atom in an S(6) loop. The dimethylsulfoxide solvent molecule accepts a strong discrete N—H⋯O hydrogen bond from the γ-lactam grouping. In the extended structure, Car—H⋯S hydrogen bonds and quasi-Type I/II Cl⋯F halogen⋯halogen bonds are observed, while adjacent dimethyl sulfoxide molecules form S⋯O chalcogen-bonded chains.Peer reviewe
CHEOPS observations of KELT-20 b/MASCARA-2 b : an aligned orbit and signs of variability from a reflective day side
Get PDFFunding: V.Si., G.Sc., G.Br., I.Pa., L.Bo., V.Na., G.Pi., R.Ra., and T.Zi. acknowledge support from CHEOPS ASI-INAF agreement no. 2019-29-HH.0. P.E.C. is funded by the Austrian Science Fund (FWF) Erwin Schroedinger Fellowship, program J4595-N. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). S.G.S. acknowledges support from FCT through FCT contract no. CEECIND/00826/2018 and POPH/FSE (EC). A.Br. was supported by the SNSA. L.Ca. and C.He. acknowledge support from the European Union H2020- MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). T.Wi. acknowledges support from the UKSA and the University of Warwick. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 through the research grants UIDB/04434/2020, UIDP/04434/2020, 2022.06962.PTDC. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. N.C.Sa. acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. Y.Al. acknowledges support from the Swiss National Science Foundation (SNSF) under grant 200020_192038. R.Al., D.Ba., E.Pa., and I.Ri. acknowledge financial support from the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación MCIN/AEI/10.13039/501100011033 and the ERDF “A way of making Europe” through projects PID2019-107061GB-C61, PID2019-107061GB-C66, PID2021-125627OB-C31, and PID2021-125627OB-C32, from the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Canarias (CEX2019-000920-S), from the Centre of Excellence “María de Maeztu” award to the Institut de Ciències de l’Espai (CEX2020-001058-M), and from the Generalitat de Catalunya/CERCA programme. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. C.Br. and A.Si. acknowledge support from the Swiss Space Office through the ESA PRODEX program. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L.D. is an F.R.S.-FNRS Postdoctoral Researcher. B.-O.D. acknowledges support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00046. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES. grant agreement no. 724427). It has also been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). D.E. acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. M.G. is an F.R.S.-FNRS Senior Research Associate. M.N.G. is the ESA CHEOPS Project Scientist and Mission Representative, and as such also responsible for the Guest Observers (GO) Programme. M.N.G. does not relay proprietary information between the GO and Guaranteed Time Observation (GTO) Programmes, and does not decide on the definition and target selection of the GTO Programme. S.H. gratefully acknowledges CNES funding through the grant 837319. K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. K.W.F.L. was supported by Deutsche Forschungsgemeinschaft grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, Exploring the Diversity of Extrasolar Planets. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. P.M. acknowledges support from STFC research grant number ST/M001040/1. Gy.M.Sz. acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Experiment Agreement No. 4000137122, the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. V.V.G. is an F.R.S-FNRS Research Associate. N.A.W. acknowledges UKSA grant ST/R004838/1. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA’s Science Mission Directorate.Context . Occultations are windows of opportunity to indirectly peek into the dayside atmosphere of exoplanets. High-precision transit events provide information on the spin-orbit alignment of exoplanets around fast-rotating hosts. Aims . We aim to precisely measure the planetary radius and geometric albedo of the ultra-hot Jupiter (UHJ) KELT-20 b along with the spin-orbit alignment of the system. Methods . We obtained optical high-precision transits and occultations of KELT-20 b using CHEOPS observations in conjunction with simultaneous TESS observations. We interpreted the occultation measurements together with archival infrared observations to measure the planetary geometric albedo and dayside temperatures. We further used the host star's gravity-darkened nature to measure the system's obliquity. Results . We present a time-averaged precise occultation depth of 82 ± 6 ppm measured with seven CHEOPS visits and 131-7+8 from the analysis of all available TESS photometry. Using these measurements, we precisely constrain the geometric albedo of KELT-20 b to 0.26 ± 0.04 and the brightness temperature of the dayside hemisphere to 2566-80+77 K. Assuming Lambertian scattering law, we constrain the Bond albedo to 0.36-0.05+0.04 along with a minimal heat transfer to the night side (ε = 0.14-0.10+0.13). Furthermore, using five transit observations we provide stricter constraints of 3 9 ± 1 1 deg on the sky-projected obliquity of the system. Conclusions . The aligned orbit of KELT-20 b is in contrast to previous CHEOPS studies that have found strongly inclined orbits for planets orbiting other A-type stars. The comparably high planetary geometric albedo of KELT-20 b corroborates a known trend of strongly irradiated planets being more reflective. Finally, we tentatively detect signs of temporal variability in the occultation depths, which might indicate variable cloud cover advecting onto the planetary day side.Peer reviewe
The salience of children increases adult prosocial values
Get PDFFunding: This study was supported by Economic and Social Research Council (grant ID: ES/P002463/1).Organizations often put children front and center in campaigns to elicit interest and support for prosocial causes. Such initiatives raise a key theoretical and applied question that has yet to be addressed directly: Does the salience of children increase prosocial motivation and behavior in adults? We present findings aggregated across eight experiments involving 2,054 adult participants: Prosocial values became more important after completing tasks that made children salient compared to tasks that made adults (or a mundane event) salient or compared to a no-task baseline. An additional field study showed that adults were more likely to donate money to a child-unrelated cause when children were more salient on a shopping street. The findings suggest broad, reliable interconnections between human mental representations of children and prosocial motives, as the child salience effect was not moderated by participants’ gender, age, attitudes, or contact with children.Peer reviewe
Design, synthesis, and photophysical properties of an iridium(III) complex bearing an indolo[3,2,1-jk]carbazole-decorated NHC ligand
Get PDFFunding: The authors would like to thank Johnson Matthey for financial support in the form of an i-CASEaward (PhD studentship to M.G.). The authors thank the University of St Andrews and EPSRC forfinancial support (grants EP/W007517/1 and EP/M02105X/1). We would like to thank theEuropean Union H2020 research and innovation program for the funding under the MarieSkłodowska-Curie Grant Agreement (PhotoReAct, No 956324).The synthesis and characterization of a novel blue-green emitting neutral heteroleptic iridium(III) complex Ir(dFppy)2(iCzmi) (λPL = 505 nm in MeCN) is reported. This represents the first example of an NHC ligand bearing an indolo-[3,2,1-jk]carbazolyl (iCz) unit, and the first use of an iCz containing ligand as the ancillary ligand in a heteroleptic Iridium(III) complex. The influence of the iCz moiety on the photophysical properties of Ir(dFppy)2(iCzmi) is explored by comparing its properties with those of the reference emitter— Ir(dFppy)2(pmi) . Both complexes show similar photophysical properties, which are rationalized in terms of a detailed computational study.Peer reviewe
Structurally and electronically driven uniaxial negative thermal expansion in BaIrO3
Get PDFFunding: We acknowledge funding from the Engineering and Physical Sciences Research Council [grant numbers EP/T011130/1 and EP/P024564/1]. Experiments at the ISIS Neutron and Muon Source were supported by a beamtime allocation RB1910632 from the Science and Technology Facilities Council.Negative thermal expansion is known to exist in a range of structure types but is extremely rare in hexagonal perovskites. Here we demonstrate that BaIrO3 displays negative linear thermal expansion in the direction of its face-shared IrO6 trimers, and apparent zero volume thermal expansion below 100 K. We present evidence that this anomalous thermal expansion is driven by an unusual form of rigid body phonon behaviour governed by the effective trimer valence state and therefore has structural and electronic components to the underlying mechanism.Peer reviewe
Design and synthesis of multi-resonant thermally activated delayed fluorescence materials and chiral emitters
No full textMulti-resonant thermally activated delayed fluorescence (MR-TADF) materials have been widely investigated as emitters in organic light-emitting diodes (OLEDs) due to their bright and narrowband emission that results from their rigid structures and short-range charge transfer (SRCT) character of the emissive excited state. However, their planar geometry and relatively large singlet-triplet energy gap lead to, respectively, severe aggregation-caused quenching (ACQ) and slow reverse intersystem crossing (RISC). This thesis is partially centered on developing new MR-TADF emitters to solve these two problems.
Using chiral compounds that can emit circularly polarized luminescence (CPL) is beneficial for their potential to increase the light out-coupling efficiency of OLEDs that use anti-glare filters. This thesis also investigates the design of chiral MR-TADF emitters, aiming to achieve bright, narrowband emission showing a strong CPL signal.
Chapter 1 introduces what is an OLED and how it works. The design of TADF emitters along with overviews of the development of heavy-atom-based MR-TADF emitters and chiral MR-TADF emitters are also discussed.
Chapter 2 presents the design of two MR-TADF emitters, TPPO-tBu-DiKTa and TPA-tBu-DiKTa, and the effect of twisted peripheral groups on the alleviation of ACQ and improvement of RISC.
Chapter 3 demonstrates two heavy-atom-based MR-TADF emitters, DiKTaSe and tBuCz-DiKTaSe, and the contribution of heavy atom effect to the TADF performance and efficiency roll-off in OLEDs.
Chapter 4 describes two chiral MR-TADF emitters tBuPh-BN and DPA-tBuPh-BN and their TADF and chiroptical properties.
Chapter 5 demonstrates the design of a propeller-shaped triple helicene DiKTa3 and explores its chiroptical properties through Density Functional Theory calculations.
Chapter 6 reports the design of a series of TADF polymers. Their TADF performance is investigated. The formation of chiral phase in polymer film through blending with chiral additives and their chiroptical properties are explored.
Chapter 7 includes the experimental methods used in this thesis."This work was supported by China Scholarship Council (Grant number 202006250026) and the School of Chemistry at the University of St Andrews."--Fundin
A step toward formalising visual data analysis practices in human computer interaction
Get PDFVisual data is an integral part of qualitative research, yet it is not always clear to researchers how to use or interpret it once gathered. Existing methods for qualitative data analysis largely rely on textual approaches such as thematic analysis, or grounded theory. Open coding is a term that is frequently used to describe a analysis that follows a logical—yet undocumented—process, but these can often be applied ad hoc, and are necessarily created after the fact of data collection. Researchers often develop their own ways of interrogating visual data, but can struggle to prove the legitimacy of not employing an existing approach. This article outlines a proven and replicable process for the analysis of static visual imagery that has been developed by the author and utilised together with research collaborators over a seven year period. The approach, which I call Annotated Visual Analysis (AVA), can be used for sketched or artistic data from participants or in first person, subjective research, in order to generate insight, gather requirements or confirm hypotheses. Here, I outline five case studies using the approach in differing contexts, in order to demonstrate its applicability, and outline the process and guidelines so that other researchers might employ the method. I also discuss the need for other researchers using visual methods to share and consolidate their forms of analysis to develop knowledge for use by others in the field.Peer reviewe
Characterisation of the warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach
Get PDFFunding: The Birmingham contribution to ASTEP+ is supported by the European Union’s Horizon 2020 research and innovation programme (grant’s agreement no. 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant no. ST/S00193X/1, and ST/W002582/1). ABr was supported by the SNSA. ACC acknowledges support from STFC consolidated grant number ST/V000861/1, and UKSA grant number ST/X002217/1. TWi acknowledges support from the UKSA and the University of Warwick. CHe acknowledges support from the European Union H2020-MSCA-ITN-2019 under Grant Agreement no. 860470 (CHAMELEON). P.M. acknowledges support from STFC research grant number ST/R000638/1. NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). N.A.W. acknowledges UKSA grant ST/R004838/1. A.H.M.J.T. acknowledges receiving funding from the Science and Technology Facilities Council (STFC; grant n° ST/S00193X/1).Context. Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as ‘lonely’ and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised. Aims. Within the contest of a multi-planet system hosting a gas giant on short orbits, we characterise the TOI-1130 system by measuring masses and orbital parameters. This is a two-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit. Methods. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data, which achieve the best precision to date on the planetary radii and masses and on the timings of each transit. Results. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision of less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively.Peer reviewe
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