Alternate Leg Bounding Acutely Improves Change of Direction Performance in Women's Team Sports Players Irrespective of Ground Type.

ABSTRACT: Dann, E, Quinn, S, Russell, M, Kilduff, LP, Turner, AN, and Hills, SP. Alternate leg bounding acutely improves change-of-direction performance in women's team sports players irrespective of ground type. J Strength Cond Res 37(6): 1199-1203, 2023-This study aimed to assess whether body mass only alternate leg bounding performed post-warm-up on grass or a hard surface acutely improves preplanned change-of-direction performance in women's team sports players relative to a control condition and, if so, profile the time course of such changes. On 3 occasions, 14 amateur women's team sports players performed 20 m preplanned change-of-direction ("Pro-Agility") tests at 4, 8, and 12 minutes after interventions. Interventions were implemented immediately after a standardized warm-up and consisted of 3 sets of 10 repetitions of alternate leg bounding (5 ground contacts per limb) on a hard indoor surface (HARD) or natural grass (GRASS), or a control condition involving approximately 75 seconds of continuous walking with no bounding (CON). Performance was similar between conditions at 4-minutes postintervention. Performance at 8 minutes was greater in HARD (2.9%, p = 0.015) and GRASS (3.8%, p = 0.029) relative to CON, whereas GRASS also exceeded CON at 12 minute post-bounding (5.2%, p = 0.004). All effects were large. No differences existed between HARD and GRASS at any time. Irrespective of the ground surface, alternate leg bounding performed with body mass only can acutely improve indices of change-of-direction performance in women's team sports players when an appropriate post-stimulus recovery period is provided. Bounding on grass or a hard surface represents a feasible match-day practice that enhances subsequent change-of-direction performance and could therefore be used as part of practically applicable pre-match, half-time, and pitch-side (re)warm-up activities.

Donor-Acceptor Dyads and Triads Employing Core-Substituted Naphthalene Diimides: A Synthetic and Spectro (Electrochemical) Study.

Donor-acceptor dyads and triads comprising core-substituted naphthalene diimide (NDI) chromophores and either phenothiazine or phenoxazine donors are described. Synthesis combined with electrochemical and spectroelectrochemical investigations facilitates characterisation of the various redox states of these molecules, confirming the ability to combine arrays of electron donating and accepting moieties into single species that retain the redox properties of these individual moieties.

Exposing the mechanisms underlying successful animal-assisted interventions for people with dementia: A realistic evaluation of the Dementia Dog Project.

There is increasing recognition of animal-assisted interventions as a promising area of practice within health and social care for people living with dementia. However, much of the research focuses on benefits for those living in care homes and not in their own homes. The Dementia Dog Project is an innovative project that aims to support people with dementia to engage with dogs and to promote the use of dogs in dementia care in the community. The pilot project introduced a dementia assistance dog to four couples where one person had a diagnosis of dementia. The aim of this paper is to explore the mechanisms that can successfully expose the benefits of integrating dogs into dementia care by drawing on the findings of a realistic evaluation of the pilot phase of the Dementia Dog Project (2013-2015). A realistic evaluation, with its focus on context, mechanisms and outcomes illuminates why an approach may work in some situations but not in others. This makes it especially appropriate to the unique, complex experience of living with dementia and the early development stage of the programme. The analysis triangulated data from a range of primary and secondary sources including interviews with the project team, case reports, team meeting notes and transcripts of interviews with participants. The findings identified three mechanisms that help to unlock the most positive outcomes for both the participants and the dogs. These were (1) the human-animal bond, (2) relationship dynamics and (3) responsibility of caring. The findings presented within this paper provide essential information to inform and advance the planning for the use of assistance dogs for people with dementia.

TESS DISCOVERY OF A TRANSITING SUPER-EARTH IN THE π MENSAE SYSTEM.

We report the detection of a transiting planet around π Men (HD 39091), using data from the Transiting Exoplanet Survey Satellite (TESS). The solar-type host star is unusually bright (V = 5.7) and was already known to host a Jovian planet on a highly eccentric, 5.7-year orbit. The newly discovered planet has a size of 2.04 ± 0.05 R ⊕ and an orbital period of 6.27 days. Radial-velocity data from the HARPS and AAT/UCLES archives also displays a 6.27-day periodicity, confirming the existence of the planet and leading to a mass determination of 4.82±0.85 M ⊕. The star's proximity and brightness will facilitate further investigations, such as atmospheric spectroscopy, asteroseismology, the Rossiter-McLaughlin effect, astrometry, and direct imaging.

Core-Substituted Naphthalene Diimides: Influence of Substituent Conformation on Strong Visible Absorption.

Functionalization of the aromatic core of naphthalene diimide (NDI) chromophores with morpholine substituents leads to molecules with strong absorbance in the visible spectrum. The shift of absorption maxima to lower energy is determined not only by the degree of substitution but also by the relative conformation and orientation of the tertiary amine with respect to the plane of the NDI.

An abundance of small exoplanets around stars with a wide range of metallicities.

The abundance of heavy elements (metallicity) in the photospheres of stars similar to the Sun provides a 'fossil' record of the chemical composition of the initial protoplanetary disk. Metal-rich stars are much more likely to harbour gas giant planets, supporting the model that planets form by accumulation of dust and ice particles. Recent ground-based surveys suggest that this correlation is weakened for Neptunian-sized planets. However, how the relationship between size and metallicity extends into the regime of terrestrial-sized exoplanets is unknown. Here we report spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission, including objects that are comparable in size to the terrestrial planets in the Solar System. We find that planets with radii less than four Earth radii form around host stars with a wide range of metallicities (but on average a metallicity close to that of the Sun), whereas large planets preferentially form around stars with higher metallicities. This observation suggests that terrestrial planets may be widespread in the disk of the Galaxy, with no special requirement of enhanced metallicity for their formation.

Kepler constraints on planets near hot Jupiters.

We present the results of a search for planetary companions orbiting near hot Jupiter planet candidates (Jupiter-size candidates with orbital periods near 3 d) identified in the Kepler data through its sixth quarter of science operations. Special emphasis is given to companions between the 21 interior and exterior mean-motion resonances. A photometric transit search excludes companions with sizes ranging from roughly two-thirds to five times the size of the Earth, depending upon the noise properties of the target star. A search for dynamically induced deviations from a constant period (transit timing variations) also shows no significant signals. In contrast, comparison studies of warm Jupiters (with slightly larger orbits) and hot Neptune-size candidates do exhibit signatures of additional companions with these same tests. These differences between hot Jupiters and other planetary systems denote a distinctly different formation or dynamical history.

Transiting circumbinary planets Kepler-34 b and Kepler-35 b.

Most Sun-like stars in the Galaxy reside in gravitationally bound pairs of stars (binaries). Although long anticipated, the existence of a 'circumbinary planet' orbiting such a pair of normal stars was not definitively established until the discovery of the planet transiting (that is, passing in front of) Kepler-16. Questions remained, however, about the prevalence of circumbinary planets and their range of orbital and physical properties. Here we report two additional transiting circumbinary planets: Kepler-34 (AB)b and Kepler-35 (AB)b, referred to here as Kepler-34 b and Kepler-35 b, respectively. Each is a low-density gas-giant planet on an orbit closely aligned with that of its parent stars. Kepler-34 b orbits two Sun-like stars every 289 days, whereas Kepler-35 b orbits a pair of smaller stars (89% and 81% of the Sun's mass) every 131 days. The planets experience large multi-periodic variations in incident stellar radiation arising from the orbital motion of the stars. The observed rate of circumbinary planets in our sample implies that more than ∼1% of close binary stars have giant planets in nearly coplanar orbits, yielding a Galactic population of at least several million.

Two Earth-sized planets orbiting Kepler-20.

Since the discovery of the first extrasolar giant planets around Sun-like stars, evolving observational capabilities have brought us closer to the detection of true Earth analogues. The size of an exoplanet can be determined when it periodically passes in front of (transits) its parent star, causing a decrease in starlight proportional to its radius. The smallest exoplanet hitherto discovered has a radius 1.42 times that of the Earth's radius (R(⊕)), and hence has 2.9 times its volume. Here we report the discovery of two planets, one Earth-sized (1.03R(⊕)) and the other smaller than the Earth (0.87R(⊕)), orbiting the star Kepler-20, which is already known to host three other, larger, transiting planets. The gravitational pull of the new planets on the parent star is too small to measure with current instrumentation. We apply a statistical method to show that the likelihood of the planetary interpretation of the transit signals is more than three orders of magnitude larger than that of the alternative hypothesis that the signals result from an eclipsing binary star. Theoretical considerations imply that these planets are rocky, with a composition of iron and silicate. The outer planet could have developed a thick water vapour atmosphere.

Kepler-16: a transiting circumbinary planet.

We report the detection of a planet whose orbit surrounds a pair of low-mass stars. Data from the Kepler spacecraft reveal transits of the planet across both stars, in addition to the mutual eclipses of the stars, giving precise constraints on the absolute dimensions of all three bodies. The planet is comparable to Saturn in mass and size and is on a nearly circular 229-day orbit around its two parent stars. The eclipsing stars are 20 and 69% as massive as the Sun and have an eccentric 41-day orbit. The motions of all three bodies are confined to within 0.5° of a single plane, suggesting that the planet formed within a circumbinary disk.

KOI-126: a triply eclipsing hierarchical triple with two low-mass stars.

The Kepler spacecraft has been monitoring the light from 150,000 stars in its primary quest to detect transiting exoplanets. Here, we report on the detection of an eclipsing stellar hierarchical triple, identified in the Kepler photometry. KOI-126 [A, (B, C)], is composed of a low-mass binary [masses M(B) = 0.2413 ± 0.0030 solar mass (M(⊙)), M(C) = 0.2127 ± 0.0026 M(⊙); radii R(B) = 0.2543 ± 0.0014 solar radius (R(⊙)), R(C) = 0.2318 ± 0.0013 R(⊙); orbital period P(1) = 1.76713 ± 0.00019 days] on an eccentric orbit about a third star (mass M(A) = 1.347 ± 0.032 M(⊙); radius R(A) = 2.0254 ± 0.0098 R(⊙); period of orbit around the low-mass binary P(2) = 33.9214 ± 0.0013 days; eccentricity of that orbit e(2) = 0.3043 ± 0.0024). The low-mass pair probe the poorly sampled fully convective stellar domain offering a crucial benchmark for theoretical stellar models.