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This study aimed to characterize Phase Change Materials (PCM) by improving their properties using shape stabilization; this was achieved by adding nanoparticles as a support material. PCM soy wax was modified using two nanoparticles, graphene, and MAXene Ti3AlC2. The synthesis process comprised stirring using a magnetic stirrer and ultrasonication using an ultrasonic processor with various percentages of 0.1, 0.5, and 1 wt.% of soy wax with nanoparticles. Based on the results, the morphologies of graphene and MAXene Ti3AlC2 were found to be in the form of sheets. These sheets had a large surface area, so soy wax could adsorb more nanoparticles to increase the stability of the material. The thermal conductivity increased with increasing percentage addition of nanoparticles. The highest values from the synthesis with graphene and MAXene Ti3AlC2 were 0.89 W/mK and 0.85 W/mK, respectively. The thermal conductivity of soy wax increased with the ratio of pure soy wax and nano-soy wax; the thermal conductivity was 6.01 for soy wax+graphene and 5.71 for soy wax+Ti3AlC2. Differential scanning calorimetry (DSC) results showed an increase in the melting and solidifying points of pure soy wax. The modified soy wax with 0.1 wt.% graphenes experienced a reduction in the melting and solidification points up to 15% and 14%, respectively. Similar results were obtained for 0.1 wt.% MAXene Ti3AlC2. In this case, there was a reduction in the melting and solidifying points by 16% and 13%, respectively. Finally, the addition of MAXene improved the material stability and thermal conductivity of soy wax and has the potential to be used as a thermal energy storage material for building applications.

Background: This study aimed to compare acceleration and deceleration demands of intercounty Camogie players, and differences across playing positions and halves of play. Hypothesis: The middle 3 positions will have greatest accelerations and decelerations variables across match play and halves of play. Study Design: Nonrandomized, repeated measures design. Level of Evidence: Level 4. Methods: Global positioning systems (GPS) (10 Hz) collected data from 28 participants during 18 competitive matches across 2 seasons; 206 individual player datasets were analyzed. Results: Half-backs (P < 0.05; effect size [ES], -1.75) and midfielders (P < 0.05; ES, -1.68) covered significantly greater total number of accelerations than full-forwards. In acceleration zone 4, midfielders (P < 0.05; ES, = -1.67) and half forwards covered a significantly greater number than full-forwards (P < 0.01; ES, = -1.41). Midfielders accumulated a significantly greater distance in acceleration zone 4 than full-backs (P < 0.05; ES, = -0.57). Significant decrements were observed between halves in total number of accelerations (P < 0.01; ES, = 0.49), accelerations in zones 1 to 4 (P < 0.01; ES, 0.16-0.43), total distance of accelerations, and acceleration distance in zones 2 to 4 (P < 0.05; ES, 0.25; P < 0.01; ES, 0.45; P < 0.01; ES, 0.38). There were significant decrements in the total number of decelerations (P < 0.01; ES, 0.43), number of decelerations in zones 2 (P < 0.05; ES, 0.25), 3 (P < 0.01; ES, 0.45), and 4 (P < 0.01; ES, 0.38), and total deceleration distance (P < 0.01; ES, 0.16). Conclusion: Half-backs and midfielders covered significantly greater total number of accelerations than full-forwards. Significant decrements in several acceleration and deceleration variables were observed between halves. Clinical Relevance: Players competing in intercounty Camogie should receive progressive exposure to acceleration and deceleration-based movement demands to prepare players for intercounty Camogie match play. [ABSTRACT FROM AUTHOR]

The aim of this study was to compare the acute effect of three cluster set (CS) intra-set rest intervals (15 s, 30 s, and 45 s) on mechanical performance measures during a flywheel resistance training session. Twelve amateur male field sport athletes attended three training measurement sessions (separated by 14 days of wash-out), consisting of four sets of nine repetitions (as cluster-blocks: 3 + 3 + 3), using a 0.050 kg·m−2 inertial load. The flywheel quarter-squat (QS) and the flywheel Romanian deadlift (RDL) were selected as resistance training exercises. Participants were randomly allocated different CS intra-set rest durations: 15 s, 30 s, or 45 s. The mean power (MP), peak concentric power (PPcon), peak eccentric power (PPecc), and eccentric overload (EO) were measured. A two-way (within–within) repeated-measures ANOVA reported that MP, PPcon, PPecc, and EO achieved similar values during the QS and RDL sessions involving 30 s and 45 s CS intra-set rest durations. It was noted that the first set did not always result in the greatest performance output for the 30 s and 45 s intervals. Compared to 15 s, the 30 s and 45 s CS intra-set rest durations showed greater MP, PPcon, and PPecc during set 2 (all p ≤ 0.05), set 3 (all p < 0.001), and set 4 (all p < 0.001) for both QS and RDL, and greater EO in the QS exercise (the four sets combined). Compared to shorter (15 s) cluster set intra-set rest intervals, longer (30–45 s) configurations allow greater physical performance outcome measures during flywheel QS and RDL resistance training sessions. The implications for longer-term interventions merit further research. [ABSTRACT FROM AUTHOR]

Antagonist static-stretching and dynamic-stretching are both effective at improving muscular performance. The purpose of this study was to investigate responses to a dynamic stretching warm-up protocol, a static-stretching warm-up protocol and a combined dynamic-stretching and antagonist static stretching warm-up protocol on isokinetic leg extension performance. Twelve participants completed a baseline (PRE) isokinetic knee-extension test at 60°.s−1 and 300°.s−1, following a 5 min warm-up on a cycle ergometer. Subsequently, participants completed the following warm-up protocols randomly over a three-week period: dynamic-stretching (DS); antagonist muscle static-stretching (AMSS) and dynamic followed by antagonist muscle static-stretching (DS-AMSS). A repeated measures analysis of variance (ANOVA) was conducted to determine where significant differences existed for peak torque, total work, average power, time-to-peak-torque and relative peak torque between warm-up protocols. DS-AMSS facilitated a significantly higher peak torque and total work compared to PRE, DS and AMSS at 60°.s−1 and 300°.s−1P < 0.05, respectively). DS-AMSS caused significantly greater relative peak torque than PRE for 60°.s−1 and 300°.s−1 (P < 0.05). DS-AMSS resulted in significantly reduced time-to-peak-torque and increased average power at 60°.s−1 compared to PRE, DS and AMSS (P < 0.05). DS-AMSS and AMSS resulted in a significant reduction in time-to-peak-torque and increased average power compared to the PRE and DS (P < 0.05) at 300°.s−1. [ABSTRACT FROM AUTHOR]

Author(s): Baojuan Ye [sup.1] , Xi Lei [sup.1] , Jianfeng Yang [sup.2] , Paul James Byrne [sup.2] , Xiaochuan Jiang [sup.3] , Mingfan Liu [sup.1] , Xinqiang Wang [sup.1] Author [...], Many university students in China find university life challenging and do not adapt well to the transition (Pan et al. 2016 (See CR72)). To address these challenges this study extends understanding of the influences of family cohesion on university students&apos; social adjustment. The study tested the mediating effect of sense of security and interpersonal disturbance. A sample of 728 Chinese university students (345 males and 383 females with a mean age of 20.62 years) was surveyed using the Family Cohesion Scale, Sense of Security Scale, Relationship Comprehensive Assessment Questionnaire, and Social Adjustment Questionnaire. The findings supported the hypotheses that family cohesion impacted social adjustment through university students&apos; sense of security and interpersonal disturbance. Family cohesion and sense of security were protective factors and disturbance in interpersonal relationship was a risk factor for social adjustment. Sense of security mediated the relationship between family cohesion and social adjustment; interpersonal disturbance mediated the relationship between family cohesion and social adjustment; sense of security and interpersonal disturbance played serial multiple mediating roles in the relationship between family cohesion and social adjustment. Application of these results might support the development of effective strategies to promote the social adjustment of university students during their transition to full adulthood.

When I started studying planetary geology I hated Venus. There's no way to see its surface directly, because the planet is wrapped in an unbroken layer of sulfuric acid clouds. [...]

The aim of this study was to determine the physical and physiological demands of intercounty camogie match-play between positions and halves of play. Data were collected from 28 players during 18 competitive games using global positioning systems (10-Hz) and heart rate monitors (2.4-GHz). The study demonstrated that intercounty camogie players covered a total distance (TD) (m ± SD) of 6,040 ± 628 m, relative distance (RD) of 83 ± 13 m⋅min-1, and maximum speed of 25 ± 1 km⋅h-1. Furthermore, the players covered a mean sprint distance of 214 ± 112 m and 14 ± 6 sprints. Players' mean heart rate (HRmean) and HRmaxwas 138 ± 23 b⋅min-1 and 164 ± 20 b⋅min-1, respectively. There were decrements between halves in TD (p < 0.01, ES = -0.45), RD (p < 0.01, ES = -0.45), maximum speed (p < 0.05, ES 5 -0.18), HRmax(p < 0.05, ES = -0.23), running (p < 0.01, ES = -0.34), high-speed running (p < 0.01, ES = 0.34), sprinting (p < 0.01, ES 5 -0.10), HRmax(p < 0.05, ES = -0.23), and HRmax % (p < 0.05, ES = -0.24). Midfielders covered a greater TD compared with full-forwards (p < 0.05, ES 5 -0.38) and half-forwards (p < 0.05, ES 5 -0.38). Full-backs covered a significantly lower RD than midfielders (p < 0.05, ES 5 -1.2), half-backs compared with full-forwards (p < 0.05, ES 5 1.14), and half-forwards compared with full-forwards (p < 0.05, ES 5 1.15). Full-forwards covered significantly less RD when compared with half-backs (p < 0.05, ES 5 -1.14), midfielders (p < 0.05, ES 5 -1.47), and half-forwards (p < 0.05, ES 5 -1.15). The findings provide physical and physiological values on the match demands of intercounty camogie match-play. [ABSTRACT FROM AUTHOR]

Previous research has proven that the balance of autistic children is poor. However, the reliability of assessing balance in this cohort has been inadequately researched. This study therefore aimed to examine if field-based static and dynamic balance tests can be reliably assessed in autistic children, to determine the number of familiarisation sessions required and whether autistic severity impacts on the reliability of these balance tests. The balance of eighteen primary school-aged autistic children was assessed three times a week over five weeks, using the flamingo balance test, a modified version of the balance error scoring system (BESS), the low beam walking test, and the heel to toe walking test. Reliability criteria included an intraclass correlation coefficient (ICC) level of ≥0.75 and a coefficient of variance (CV%) of ≤46% for the low beam walking test, the heel to toe walking test, and the BESS, and a CV% of ≤82% or the flamingo balance test. Inter-session reliability was achieved and required the least number of familiarisation sessions for the flamingo balance test, compared to the low beam walking test, which required a greater number of familiarisation sessions to achieve inter-session reliability. The heel to toe walking test and the BESS achieved inter-session reliability and familiarisation in an acceptable time frame. Due to the large CV% values reported in the current study, practitioners need to be aware that balance interventions need to achieve improvements greater than the CV% in this cohort. [ABSTRACT FROM AUTHOR]

The heavily faulted Martian terrains of Ceraunius Fossae and Tractus Fossae, south of the Alba Mons volcano, have previously only been considered as parts of larger tectonic studies of Alba Mons, and consequently the complexity of the faulting remains unclear. As these terrains are in the midst of the large Tharsis volcanoes, the study of their surface deformation has the potential to help unravel the volcano‐tectonic deformation associated with the growth of Tharsis as well as to decipher details of the magma‐tectonic processes responsible for graben formation. Here, we distinguish between faults and collapse structures based on image and topographic evidence. We mapped ∼12,000 faults, which we grouped into three distinct fault groups based on orientation, morphology, and relative ages. These show a temporal evolution in the mapped fault orientations from NE to N‐S to NW with associated changes in stress orientations. We also mapped collapse features and categorized them into four different groups: pit‐crater chains, catenae, u‐shaped troughs and chasmata. Examining the four collapse structure groups reveals that they are likely four progressive stages in the erosional evolution of pit‐crater chains. Together, this revealed a structural history heavily influenced by lateral diking from both local (radial to Alba Mons, Pavonis Mons and Ascraeus Mons) and regional (radial to Tharsis) sources, and vertical diking from a proposed Ceraunius Fossae centered magma source. This, along with an updated crater size‐frequency distribution analysis of the unit ages, reveals a highly active tectonic and magmatic environment south of Alba Mons in the Middle Amazonian. Plain Language Summary: The large‐scale faults surrounding the dome of the Alba Mons volcano on Mars have been studied intensely, while the faulted area south of Alba Mons has received relatively little attention. Closer inspection of these southern terrains, namely Ceraunius Fossae and Tractus Fossae, reveals that this area is far more complex in structure and more recent in activity than previously thought. In this study, we mapped and measured all the faults in the study areas. In addition to the faults, the surface of the study area is covered in "collapse structures." These are circular to trough‐like features created when the surface material has fallen into a subsurface cavity. We mapped and characterized these faults and collapse structures, in order to determine the history of events and which geological process created them. We found three distinct extensional faulting events, and examples of four types of collapse structures. These events all took place within 2.4–1.4 billion years ago during the Amazonian period. Together, these results show that magmatic activity drove structure deformation, both from the surrounding Alba Mons, Ascraeus Mons and Pavonis Mons volcanoes, and also from a local large magmatic source situated directly underneath Ceraunius Fossae. Key Points: Three fault populations and four types of collapse features are mapped and analyzed in Ceraunius Fossae and Tractus FossaeWe present a four‐stage structural evolution of the area, with dike‐induced deformation being the prevalent processThe stages of activity in the study area all occurred during the Amazonian, with activity from a local magmatic source beneath Ceraunius Fossae [ABSTRACT FROM AUTHOR]

This study presents a comprehensive assessment of the geomorphology, crater distributions, and tectonic structures within Enceladus' cratered terrains. We analyzed the distributions of impact craters and tectonic structures in seven regions of interest to inform an interpretation of the geological history of this terrain in the context of Enceladus' global evolution. We found that the tectonic structures, including both ancient, subdued troughs and young, narrow fractures, point to a cratered terrain that not only experienced early tectonic modification but also shows evidence of recent geological activity. Ancient troughs present in the equatorial cratered terrains are similar in scale and orientation to troughs present in the Leading and Trailing Hemisphere Terrains, an observation that supports possible non‐synchronous rotation of the ice shell. A dearth of impact craters in the equatorial regions as identified previously does not hold for craters <3 km in diameter in the anti‐Saturnian hemisphere. The anomalous presence of excess small craters in this region could be due to secondary or sesquinary impacts from a catastrophic event occurring at Enceladus or a neighboring moon. Finally, narrow fractures are pervasive across the cratered terrains and are most commonly oriented parallel or sub‐parallel to the most proximal cratered terrain boundary. This directionality of pervasive recent fracturing could be related to the vertical movement of an isostatically uncompensated ice shell. Enceladus' cratered terrains provide insight into the long‐term evolution of the satellite, an important component to assessing its role in Solar System evolution and its potential for habitability. Plain Language Summary: We present a comprehensive characterization of the oldest terrain on Enceladus, the cratered terrains. We evaluated structural features and impact craters on the surface, including their morphology and spatial distributions. This analysis informs how we interpret the formation and change of these surface features in the context of how Enceladus as a whole has changed over time. We found that there are two main types of tectonic structures in the cratered terrains, including one set of relatively old troughs and at least one set of narrow fractures that is very young. This finding indicates that not only have the cratered terrains experienced early tectonic activity, but were also active recently. The ancient set of troughs are similar to those present in younger terrains on Enceladus, suggesting that the ice shell has rotated relative to its tidally locked position about Saturn. The comparatively young, narrow fractures in the cratered terrains are widespread and could have formed due to a vertically shifting ice shell. Enceladus' cratered terrains provide insight into what long‐term changes have taken place on the surface, an important component to understanding how Enceladus fits into Solar System formation and its past or present potential to host life. Key Points: Systematic review of Enceladus' cratered terrains results in a stratigraphic framework for geologic mapping and age determinationTroughs in the equatorial cratered terrains are similar to tectonized equatorial regions, suggesting non‐synchronous ice shell rotationAncient, subdued troughs and young, narrow fractures point to a cratered terrain that experienced both early and recent tectonic activity [ABSTRACT FROM AUTHOR]

Although Earth is the only known planet on which plate tectonics operates, many small- and large-scale tectonic landforms indicate that deformational processes also occur on the other rocky planets. Although the mechanisms of deformation differ on Mercury, Venus, and Mars, the surface manifestations of their tectonics are frequently very similar to those found on Earth. Furthermore, tectonic processes invoked to explain deformation on Earth before the recognition of horizontal mobility of tectonic plates remain relevant for the other rocky planets. These connections highlight the importance of drawing analogies between the rocky planets for characterizing deformation of their lithospheres and for describing, applying appropriate nomenclature, and understanding the formation of their resulting tectonic structures. Here we characterize and compare the lithospheres of the rocky planets, describe structures of interest and where we study them, provide examples of how historic views on geology are applicable to planetary tectonics, and then apply these concepts to Mercury, Venus, and Mars. Key words: planetary tectonics, planetary geology, Mercury, Venus, Mars. Bien que la Terre soit la seule planete connue sur laquelle il y a une tectonique des plaques, de nombreuses formes de relief tectoniques de petite et grande envergure indiquent que des processus de deformation se produisent egalement sur d'autres planetes rocheuses. Si les mecanismes de deformation sur Mercure, Venus et Mars different, les manifestations en surface de leurs tectoniques respectives sont souvent tres semblables a celles observees sur la Terre. En outre, des processus tectoniques invoques pour expliquer la deformation sur la Terre avant la reconnaissance de la mobilite horizontale de plaques tectoniques revetent toujours une pertinence pour les autres planetes rocheuses. Ces connexions soulignent l'importance d'etablir des analogies entre les planetes rocheuses pour caracteriser la deformation de leurs lithospheres et pour decrire, en appliquant la bonne nomenclature, et comprendre la formation des structures tectoniques en resultant. Nous caracterisons et comparons les lithospheres des planetes rocheuses, decrivons les structures d'interet et les lieux ou elles sont etudiees, et presentons des exemples d'application de notions historiques a la tectonique planetaire pour ensuite appliquer ces concepts a Mercure, Venus et Mars. [Traduit par la Redaction] Mots-cles: tectonique des planetes, geologie des planetes, Mercure, Venus, Mars., Introduction Without a theoretical framework, such as the plate tectonic models, of the spatial relations of rock bodies to one another in an orogenic belt, however wrong they may be, [...]