Predictors of upper extremity symptoms and functional impairment among workers employed for 6 months in a new job

Background We sought to identify personal and work-related predictors of upper extremity symptoms and related functional impairment among 1,108 workers employed for 6 months in a new job. Methods We collected data at baseline and 6-month follow-up using self-administered questionnaires. Multivariate logistic regression models were created for each outcome variable. Predictors included personal risk factors, physical work exposures and psychosocial factors. Results Independent predictors for upper extremity symptoms at 6-month follow-up were age, Caucasian race, female gender, baseline history of UE symptoms, and job tasks involving wrist bending or forceful gripping. Independent predictors for functional impairment were baseline history and severity of UE symptoms, wrist bending, and social support. Conclusions Both personal and work-related factors were independent predictors of upper extremity symptoms and functional impairment in this working population. We found different risk factors for symptoms than for functional impairment related to symptoms. Am. J. Ind. Med. 51:932–940, 2008. © 2008 Wiley-Liss, Inc.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/61341/1/20625_ftp.pd

Pulsations in main sequence OBAF-type stars

CONTEXT: The third Gaia data release provides photometric time series covering 34 months for about 10 million stars. For many of those stars, a characterisation in Fourier space and their variability classification are also provided. This paper focuses on intermediate- to high-mass (IHM) main sequence pulsators (M ≥  1.3 M⊙) of spectral types O, B, A, or F, known as β Cep, slowly pulsating B (SPB), δ Sct, and γ Dor stars. These stars are often multi-periodic and display low amplitudes, making them challenging targets to analyse with sparse time series. AIMS: We investigate the extent to which the sparse Gaia DR3 data can be used to detect OBAF-type pulsators and discriminate them from other types of variables. We aim to probe the empirical instability strips and compare them with theoretical predictions. The most populated variability class is that of the δ Sct variables. For these stars, we aim to confirm their empirical period-luminosity (PL) relation, and verify the relation between their oscillation amplitude and rotation. METHODS: All datasets used in this analysis are part of the Gaia DR3 data release. The photometric time series were used to perform a Fourier analysis, while the global astrophysical parameters necessary for the empirical instability strips were taken from the Gaia DR3 gspphot tables, and the v sin i data were taken from the Gaia DR3 esphs tables. The δ Sct PL relation was derived using the same photometric parallax method as the one recently used to establish the PL relation for classical Cepheids using Gaia data. RESULTS: We show that for nearby OBAF-type pulsators, the Gaia DR3 data are precise and accurate enough to pinpoint them in the Hertzsprung-Russell (HR) diagram. We find empirical instability strips covering broader regions than theoretically predicted. In particular, our study reveals the presence of fast rotating gravity-mode pulsators outside the strips, as well as the co-existence of rotationally modulated variables inside the strips as reported before in the literature. We derive an extensive period–luminosity relation for δ Sct stars and provide evidence that the relation features different regimes depending on the oscillation period. We demonstrate how stellar rotation attenuates the amplitude of the dominant oscillation mode of δ Sct stars. CONCLUSIONS: The Gaia DR3 time-series photometry already allows for the detection of the dominant (non-)radial oscillation mode in about 100 000 intermediate- and high-mass dwarfs across the entire sky. This detection capability will increase as the time series becomes longer, allowing the additional delivery of frequencies and amplitudes of secondary pulsation modes

Gaia Data Release 3 Pulsations in main sequence OBAF-type stars

Context. The third Gaia data release provides photometric time series covering 34 months for about 10 million stars. For many of those stars, a characterisation in Fourier space and their variability classification are also provided. This paper focuses on intermediate- to high-mass (IHM) main sequence pulsators (M ≥  1.3 M⊙) of spectral types O, B, A, or F, known as β Cep, slowly pulsating B (SPB), δ Sct, and γ Dor stars. These stars are often multi-periodic and display low amplitudes, making them challenging targets to analyse with sparse time series. Aims. We investigate the extent to which the sparse Gaia DR3 data can be used to detect OBAF-type pulsators and discriminate them from other types of variables. We aim to probe the empirical instability strips and compare them with theoretical predictions. The most populated variability class is that of the δ Sct variables. For these stars, we aim to confirm their empirical period-luminosity (PL) relation, and verify the relation between their oscillation amplitude and rotation. Methods. All datasets used in this analysis are part of the Gaia DR3 data release. The photometric time series were used to perform a Fourier analysis, while the global astrophysical parameters necessary for the empirical instability strips were taken from the Gaia DR3 gspphot tables, and the v sin i data were taken from the Gaia DR3 esphs tables. The δ Sct PL relation was derived using the same photometric parallax method as the one recently used to establish the PL relation for classical Cepheids using Gaia data. Results. We show that for nearby OBAF-type pulsators, the Gaia DR3 data are precise and accurate enough to pinpoint them in the Hertzsprung-Russell (HR) diagram. We find empirical instability strips covering broader regions than theoretically predicted. In particular, our study reveals the presence of fast rotating gravity-mode pulsators outside the strips, as well as the co-existence of rotationally modulated variables inside the strips as reported before in the literature. We derive an extensive period–luminosity relation for δ Sct stars and provide evidence that the relation features different regimes depending on the oscillation period. We demonstrate how stellar rotation attenuates the amplitude of the dominant oscillation mode of δ Sct stars. Conclusions. The Gaia DR3 time-series photometry already allows for the detection of the dominant (non-)radial oscillation mode in about 100 000 intermediate- and high-mass dwarfs across the entire sky. This detection capability will increase as the time series becomes longer, allowing the additional delivery of frequencies and amplitudes of secondary pulsation modes

Lessons learned from the perinatal audit of uterine rupture in the Netherlands: A mixed‐method study

Abstract Background and Aims To analyze outcomes of nationwide local audits of uterine rupture to draw lessons for clinical care. Methods Descriptive cohort study. Critical incident audit sessions within all local perinatal cooperation groups in the Netherlands. Women who sustained uterine rupture between January 1st, 2017 and December 31st, 2019. Main Outcome Measures Improvable factors, recommendations, and lessons learned for clinical care. Women's case histories were discussed in multidisciplinary perinatal audit sessions. Participants evaluated care against national and local clinical guidelines and common professional standards to identify improvable factors. Cases and outcomes were registered in a nationwide database. Results One hundred and fourteen women who sustained uterine rupture were discussed in local perinatal audit sessions by 40–60 participants on average: A total of 111 (97%) were multiparous of whom 107 (94%) had given birth by cesarean section in a previous pregnancy. The audit revealed 178 improvable factors and 200 recommendations. Six percent (N = 11) of the improvable factors were identified as very likely and 18% (N = 32) as likely to have a relationship with the outcome or occurrence of uterine rupture. Improvable factors were related to inadequate communication, absent, or unclear documentation, delay in diagnosing the rupture, and suboptimal management of labor. Speak up in case a suspicion arises, escalating care by involving specialist obstetricians, addressing the importance of accurate documentation, and improving training related to fetal monitoring were the most frequent recommendations and should be topics for team (skills and drills) training. Conclusions Through a nationwide incident audit of uterine rupture, we identified improvable factors related to communication, documentation, and organization of care. Lessons learned include “speaking up,” improving the transfer of information and team training are crucial to reduce the incidence of uterine rupture