The finite temperature Brueckner-Hartree-Fock approach is extended by introducing a microscopic three-body force. In the framework of the extended model, the equation of state of hot asymmetric nuclear matter and its isospin dependence have been investigated. The critical temperature of liquid-gas phase transition for symmetric nuclear matter has been calculated and compared with other predictions. It turns out that the three-body force gives a repulsive contribution to the equation of state which is stronger at higher density and as a consequence reduces the critical temperature of liquid-gas phase transition. The calculated energy per nucleon of hot asymmetric nuclear matter is shown to satisfy a simple quadratic dependence on asymmetric parameter β as in the zero-temperature case. The symmetry energy and its density dependence have been obtained and discussed. Our results show that the three-body force affects strongly the high-density behavior of the symmetry energy and makes the symmetry energy more sensitive to the variation of temperature. The temperature dependence and the isospin dependence of other physical quantities, such as the proton and neutron single particle potentials and effective masses are also studied. Due to the additional repulsion produced by the three-body force contribution, the proton and neutron single particle potentials are correspondingly enhanced as similar to the zerotemperature case.

The Caprini RAM was suggested to be more effective than the Padua RAM for identification of hospitalized medical patients at risk for VTE.

Aims To investigate the mental workload level of nurses aiding the most affected area during the Coronavirus disease 2019 (COVID‐19) pandemic and explore the subtypes of nurses regarding their mental workload. Design Cross‐sectional study. Methods A sample of 446 frontline nurses participated from March 8 to 19, 2020. A latent profile analysis was performed to identify clusters based on the six subscales of the Chinese version of the National Aeronautics and Space Administration Task Load Index . The differences among the classes and the variables including sociodemographic characteristics, psychological capital and coping style were explored. Results The level of mental workload indicates that the nurses had high self‐evaluations of their performance while under extremely intensive task loads. The following three latent subtypes were identified: ‘low workload & low self‐evaluation’ (8.6%); ‘medium workload & medium self‐evaluation’ (35.3%) and ‘high workload & high self‐evaluation’ (56.1%) ( Classes 1 , 2 , and 3 , respectively). Nurses with shared accommodations, fewer years of practice, junior professional titles, lower incomes, nonmanagement working positions, lower psychological capital levels and negative coping styles had a higher likelihood of belonging to Class 1 . In contrast, senior nurses with higher psychological capital and positive coping styles were more likely to belong to Classes 2 and 3 . Conclusion The characteristics of the ‘low workload & low self‐evaluation’ subtype suggest that attention should be paid to the work pressure and psychological well‐being of junior nurses. Further research on regular training program of public health emergency especially for novices is needed. Personnel management during public health events should be focused on the allocation between novice and senior frontline nurses. Impact This study addresses the level of mental workload of frontline nurses who aid in the most severe area of the COVID‐19 pandemic in China and delineates the characteristics of the subtypes of these nurses.

We investigate the effect of a microscopic three-body force on the proton and neutron superfluidity in the 1 S 0 channel in β-stable neutron star matter. It is found that the three-body force has only a small effect on the neutron 1 S 0 pairing gap, but it suppresses strongly the proton 1 S 0 superfluidity in β-stable neutron star matter.PACS numbers: 26.60.+c,21.65.+f, 21.30.FeKeywords: 1 S 0 superfluidity, three-body Force, β-stable neutron star matter, Brueckner-Hartree-Fock approachSuperfluidity plays an important role in understanding a number of astrophysical phenomena in neutron stars [1][2][3][4][5][6][7][8][9][10]. It is generally expected that the cooling processes via neutrino emission [5,6,7], the properties of rotating dynamics, the post-glitch timing observations [8,9], the possible vertex pinning [10] of a neutron star are rather sensitive to the presence of neutron and proton superfluid phases as well as to their