Dynamic skeletal traction spica casts for paediatric femoral fractures in a resource-limited setting

The objective of this study was to compare elastic intramedullary nailing (EIN) with dynamic skeletal traction spica casting (DSTSC) in terms of postoperative radiographic angulations, length of hospital stay, and cost in a resource-limited setting. We prospectively studied 51 children, five to twelve years of age, with femoral fractures treated with either EIN (n = 26) or DSTSC (n = 25). Children treated with EIN had significantly longer hospital stays (17 ± 8.0 days) than those treated with DSTSC (6.0 ± 2.5 days). Financial constraints in acquiring supplies caused a significant increase in time from admission to surgery (EIN 9.5 ± 2.3 days; DSTSC 1.1 ± 0.3 days), and cost was about 400% higher for EIN compared with DSTSC. At twelve weeks follow-up, all patients in both groups had acceptable radiographic angulations. In resource-limited healthcare settings, DSTSC is an effective alternative to EIN with comparable post-op radiographic angulations, decreased hospital stays, and lower cost

Model comparison from LIGO–Virgo data on GW170817’s binary components and consequences for the merger remnant

GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05 M-circle dot, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67 M-circle dot for the case that the merger results in a hypermassive neutron star