An Exploration of Coaches’ and Sport Psychologists’ Experiences of Managing Performance Blocks

This study examined coaches’ and sport psychologists’ experiences of managing performance blocks and the mechanisms they adopted in supporting athletes who experience them. This qualitative study adopted a constructivist philosophical paradigm. Semi-structured interviews were conducted with elite coaches (n=8) and HCPC-registered sport psychologists (n=7). Following transcription, interviews were analyzed using thematic analysis (Braun & Clarke, 2006, 2021). Findings indicated that managing performance blocks is a complex and dynamic process whereby participants iteratively moved through five stages (i.e., understanding the athlete, intervening in performance blocks, experiencing the emotional rollercoaster, coping with emotions, and learning). From an applied perspective, findings encourage coaches and sport psychologists to create trusting relationships with the athlete and demonstrate an emotional understanding of athletes’ needs. Findings indicate that lowering the psychological demand and increasing the athletes’ coping resources such as by offering emotional support is an important strategy in the management of performance blocks. Lay Summary: This article explores eight coaches’ and seven sport psychologists’ experiences of managing performance blocks. Coaches and sport psychologists continually shifted between five stages in understanding and supporting athletes’ experiences of performance blocks. Findings highlight the importance of trusting and collaborative relationships, emotional intelligence, and coping strategies when managing performance blocks. Applied Implications: • Coaches and sport psychologists must create and maintain trusting relationships with the athlete and those surrounding the athlete before attempting to intervene in performance blocks to ensure athletes feel safe in discussing performance blocks and receive consistent and supportive messaging. • Coaches and sport psychologists are encouraged to develop and utilize effective coping strategies throughout managing performance blocks. Examples including seeking support from colleagues and supervisors, participating in reflective practice, and seeking emotional support from friends and family. • Sporting organizations can improve the management of performance blocks by providing coach education sessions to raise awareness of the causes and warning signs, and highlight instances of best and worst practice for management

An exploration of coaches’ and sport psychologists’ experiences of managing performance blocks

This study examined coaches’ and sport psychologists’ experiences of managing performance blocks and the mechanisms they adopted in supporting athletes who experience them. This qualitative study adopted a constructivist philosophical paradigm. Semi-structured interviews were conducted with elite coaches (n = 8) and HCPC-registered sport psychologists (n = 7). Following transcription, interviews were analyzed using thematic analysis. Findings indicated that managing performance blocks is a complex and dynamic process whereby participants iteratively moved through five stages (i.e., understanding the athlete, intervening in performance blocks, experiencing the emotional rollercoaster, coping with emotions, and learning). From an applied perspective, findings encourage coaches and sport psychologists to create trusting relationships with the athlete and demonstrate an emotional understanding of athletes’ needs. Findings indicate that lowering the psychological demand and increasing the athletes’ coping resources such as by offering emotional support is an important strategy in the management of performance blocks. Lay summary: This article explores eight coaches’ and seven sport psychologists’ experiences of managing performance blocks. Coaches and sport psychologists continually shifted between five stages in understanding and supporting athletes’ experiences of performance blocks. Findings highlight the importance of trusting and collaborative relationships, emotional intelligence, and coping strategies when managing performance blocks.Applied implications Coaches and sport psychologists must create and maintain trusting relationships with the athlete and those surrounding the athlete before attempting to intervene in performance blocks to ensure athletes feel safe in discussing performance blocks and receive consistent and supportive messaging. Coaches and sport psychologists are encouraged to develop and utilize effective coping strategies throughout managing performance blocks. Examples including seeking support from colleagues and supervisors, participating in reflective practice, and seeking emotional support from friends and family. Sporting organizations can improve the management of performance blocks by providing coach education sessions to raise awareness of the causes and warning signs, and highlight instances of best and worst practice for management

Predicting Ares I Reaction Control System Performance by Utilizing Analysis Anchored with Development Test Data

The Ares I launch vehicle is an integral part of NASA s Constellation Program, providing a foundation for a new era of space access. The Ares I is designed to lift the Orion Crew Module and will enable humans to return to the Moon as well as explore Mars.1 The Ares I is comprised of two inline stages: a Space Shuttle-derived five-segment Solid Rocket Booster (SRB) First Stage (FS) and an Upper Stage (US) powered by a Saturn V-derived J-2X engine. A dedicated Roll Control System (RoCS) located on the connecting interstage provides roll control prior to FS separation. Induced yaw and pitch moments are handled by the SRB nozzle vectoring. The FS SRB operates for approximately two minutes after which the US separates from the vehicle and the US Reaction Control System (ReCS) continues to provide reaction control for the remainder of the mission. A representation of the Ares I launch vehicle in the stacked configuration and including the Orion Crew Exploration Vehicle (CEV) is shown in Figure 1. Each Reaction Control System (RCS) design incorporates a Gaseous Helium (GHe) pressurization system combined with a monopropellant Hydrazine (N2H4) propulsion system. Both systems have two diametrically opposed thruster modules. This architecture provides one failure tolerance for function and prevention of catastrophic hazards such as inadvertent thruster firing, bulk propellant leakage, and over-pressurization. The pressurization system on the RoCS includes two ambient pressure-referenced regulators on parallel strings in order to attain the required system level single Fault Tolerant (FT) design for function while the ReCS utilizes a blow-down approach. A single burst disk and relief valve assembly is also included on the RoCS to ensure single failure tolerance for must-not-occur catastrophic hazards. The Reaction Control Systems are designed to support simultaneously firing multiple thrusters as require

INTEGRAL-ISGRI observations of the CygOB2 region: earching for hard X-ray point sources in a region containing several non-thermal emitting massive stars

Aims: We analyze INTEGRAL-ISGRI data in order to probe the hard X-ray emission (above 20 keV) from point sources in the Cyg OB2 region and to investigate the putative non-thermal high-energy emission from early-type stars (Wolf-Rayet and O-type stars). Among the targets located in the field of view, we focus on the still unidentified EGRET source 3EG 2033+4118 that may be related to massive stars known to produce non-thermal emission in the radio domain, and on the wide colliding-wind binary WR 140. Methods: Using a large set of data obtained with the IBIS-ISGRI imager onboard INTEGRAL, we run the OSA software package in order to find point sources in the fully coded field of view of the instrument. Results: Our data do not allow the detection of a lower-energy counterpart of 3EG J2033+4118 nor of any other new point sources in the field of view, and we derive upper limits on the high-energy flux for a few targets: 3EG J2033+4118, TeV J2032+4130, WR140, WR146 and WR147. The results are discussed in the context of the multiwavelength investigation of these objects. Conclusions: The upper limits derived are valuable constraints for models aimed at understanding the acceleration of particles in non-thermal emitting massive stars, and of the still unidentified very-high gamma-ray source TeV J2032+4130.Comment: 6 page, 2 figures including one figure in GIF format, accepted for publication by A&

Chandra ACIS Survey of M33 (ChASeM33): The enigmatic X-ray emission from IC131

We present the first X-ray analysis of the diffuse hot ionized gas and the point sources in IC131, after NGC604 the second most X-ray luminous giant HII region in M33. The X-ray emission is detected only in the south eastern part of IC131 (named IC131-se) and is limited to an elliptical region of ~200pc in extent. This region appears to be confined towards the west by a hemispherical shell of warm ionized gas and only fills about half that volume. Although the corresponding X-ray spectrum has 1215 counts, it cannot conclusively be told whether the extended X-ray emission is thermal, non-thermal, or a combination of both. A thermal plasma model of kT_e=4.3keV or a single power law of Gamma=2.1 fit the spectrum equally well. If the spectrum is purely thermal (non-thermal), the total unabsorbed X-ray luminosity in the 0.35-8keV energy band amounts to L_X = 6.8(8.7)x10^35erg/s. Among other known HII regions IC131-se seems to be extreme regarding the combination of its large extent of the X-ray plasma, the lack of massive O stars, its unusually high electron temperature (if thermal), and the large fraction of L_X emitted above 2keV (~40-53%). A thermal plasma of ~4keV poses serious challenges to theoretical models, as it is not clear how high electron temperatures can be produced in HII regions in view of mass-proportional and collisionless heating. If the gas is non-thermal or has non-thermal contributions, synchrotron emission would clearly dominate over inverse Compton emission. It is not clear if the same mechanisms which create non-thermal X-rays or accelerate CRs in SNRs can be applied to much larger scales of 200pc. In both cases the existing theoretical models for giant HII regions and superbubbles do not explain the hardness and extent of the X-ray emission in IC131-se.Comment: 28 pages, 7 figures and 2 tables. Accepted for publication in ApJ. For a high resolution version of the paper see http://hea-www.harvard.edu/vlp_m33_public/publications.htm

Anaesthetists stress is induced by patient ASA grade and may impair non-technical skills during intubation

BackgroundThe aims of this study were to determine if patient ASA grade was associated with increased stress in anaesthetists with a subsequent effect on non-technical skills.MethodsStress was measured using a validated objective (heart rate variability or heart rate) and subjective tool. We studied eight consultant anaesthetists at baseline (rest) and during 16 episodes of intubation with an ASA 1 or 2 patient vs. an ASA 3 or 4 patient. The primary outcome for the study was objective and subjective stress between both patient groups. Secondary outcomes were non-technical skill ratings and the association between stress measurements.ResultsASA 3 or 4 patients were associated with increases in objective stress when compared to baseline (mean 4.6 vs. 6.7; P = 0.004). However, ASA 1 or 2 patients were not associated with increases in stress when compared to baseline (mean 4.6 vs. 4.7; P = 1). There was no significant difference in subjective stress between the groups (P = 0.18). Objective stress negatively affected situational awareness (P = 0.03) and decision-making (P = 0.03); however, these did not decline to a clinically significant threshold. Heart rate variability (r = 0.60; P = 0.002) better correlated with subjective stress when compared to heart rate (r = 0.30; P = 0.15). Agreement between raters for Anaesthetic Non-Technical Skills (ANTS) scores was acceptable (ICC = 0.51; P = 0.003).ConclusionThis study suggests that higher patient ASA grade can increase stress in anaesthetists, which may impair non-technical skills

Multiwavelength Observations of LS I +61 303 with VERITAS, Swift and RXTE

We present results from a long-term monitoring campaign on the TeV binary LSI +61 303 with VERITAS at energies above 500 GeV, and in the 2-10 keV hard X-ray bands with RXTE and Swift, sampling nine 26.5 day orbital cycles between September 2006 and February 2008. The binary was observed by VERITAS to be variable, with all integrated observations resulting in a detection at the 8.8 sigma (2006/2007) and 7.3 sigma (2007/2008) significance level for emission above 500 GeV. The source was detected during active periods with flux values ranging from 5 to 20% of the Crab Nebula, varying over the course of a single orbital cycle. Additionally, the observations conducted in the 2007-2008 observing season show marginal evidence (at the 3.6 sigma significance level) for TeV emission outside of the apastron passage of the compact object around the Be star. Contemporaneous hard X-ray observations with RXTE and Swift show large variability with flux values typically varying between 0.5 and 3.0*10^-11 ergs cm^-2 s^-1 over a single orbital cycle. The contemporaneous X-ray and TeV data are examined and it is shown that the TeV sampling is not dense enough to detect a correlation between the two bands.Comment: 30 pages, 5 figures, 2 table, Accepted for publication in The Astrophysical Journa

Sustained release of decorin to the surface of the eye enables scarless corneal regeneration

Ophthalmology: novel eye drop brings sustained drug delivery to ocular surface An eye drop formulation that applies anti-scarring drugs to the surface of the eye helps reverse infection-induced corneal damage in mice. Hill et al. from the University of Birmingham, UK, formulated a fluid gel loaded with a wound-healing protein called decorin that conforms to the ocular surface and is cleared gradually through blinking. With colleagues in California, they applied the therapeutic eye drop to mice with bacterial eye infections that trigger sight-threatening corneal scarring. Within a matter of days, the team saw improvements in corneal transparency, with reductions in scar tissue and reconstitution of healthy cells. Such a drug delivery system, if successful in humans, could help save many people’s sight and reduce the need for corneal transplantation

VERITAS Observations of the gamma-Ray Binary LS I +61 303

LS I +61 303 is one of only a few high-mass X-ray binaries currently detected at high significance in very high energy gamma-rays. The system was observed over several orbital cycles (between September 2006 and February 2007) with the VERITAS array of imaging air-Cherenkov telescopes. A signal of gamma-rays with energies above 300 GeV is found with a statistical significance of 8.4 standard deviations. The detected flux is measured to be strongly variable; the maximum flux is found during most orbital cycles at apastron. The energy spectrum for the period of maximum emission can be characterized by a power law with a photon index of Gamma=2.40+-0.16_stat+-0.2_sys and a flux above 300 GeV corresponding to 15-20% of the flux from the Crab Nebula.Comment: accepted for publication in The Astrophysical Journa

VERITAS Observations of the BL Lac Object 1ES 1218+304

The VERITAS collaboration reports the detection of very-high-energy (VHE) gamma-ray emission from the high-frequency-peaked BL Lac object 1ES 1218+304 located at a redshift of z=0.182. A gamma-ray signal was detected with high statistical significance for the observations taken during several months in the 2006-2007 observing season. The photon spectrum between ~160 GeV and ~1.8 TeV is well described by a power law with an index of Gamma = 3.08 +/- 0.34(stat) +/- 0.2(sys). The integral flux above 200 GeV corresponds to ~6% of that of the Crab Nebula. The light curve does not show any evidence for VHE flux variability. Using lower limits on the density of the extragalactic background light (EBL) in the near-IR to mid-IR we are able to limit the range of intrinsic energy spectra for 1ES 1218+304. We show that the intrinsic photon spectrum is harder than a power law with an index of Gamma = 2.32 +/- 0.37. When including constraints from the spectra of 1ES 1101-232 and 1ES 0229+200, the spectrum of 1ES 1218+304 is likely to be harder than Gamma = 1.86 +/- 0.37.Comment: Submitted to Proceedings of "4th Heidelberg International Symposium on High Energy Gamma-Ray Astronomy 2008