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Background: Optimal communication and collaboration between inter-disciplinary health care providers is critical to ensuring high quality patient care. We aimed to quantify the impact on physician-nurse collaboration (PNC) of implementing daily goal sheets (DGSs) in emergency settings. Methods: The usage of a DGS was administered in morning rounds in an emergency intensive care unit (ICU) for four consecutive months. A Jefferson Scale of Attitudes Toward Physician-Nurse Collaboration (JSAPNC) form was used before (n=113) and after (n=107) the intervention to evaluate the attitudes of PNCs from the perspective of both physicians and nurses. Results: There is a significant positive relation between the attitude to PNC and the participant age, educational background, and professional rank and title before DGS application (P

In this paper, we report the new results of spectroscopic observations of $\gamma$-ray blazar S5 0716+714 from 2019 September to 2020 March with the 2.4 m optical telescope at Lijiang Observatory of Yunnan Observatories. The median cadence of observations is $\sim$ 1 day. During the second observation period (Epoch2), the observational data reveal an extremely bright state and a bluer-when-brighter (BWB) chromatism. The BWB trend of Epoch2 differs significantly from that of the first observation period (Epoch1). A significantly brightness-dependent BWB chromatism emerges in the total data of Epoch1 and Epoch2. The BWB trend becomes weaker towards the brighter states, and likely becomes saturated at the highest state. Based on a log-parabolic function, a power-law of synchrotron peak flux and frequency $\nu_{\rm{p}}$, and a power-law of the curvature of synchrotron spectrum and its $\nu_{\rm{p}}$, simulation well reproduces the brightness-dependent BWB trend of S5 0716+714. The BWB trend is seemingly controlled by the shift of $\nu_{\rm{p}}$ with respect to the observational window, and effectively may be dominated by the variations of electron average energy and magnetic field in emitting region., Comment: 16 pages, 5 figures, Accepted for publication in ApJ

The changes of broad emission lines should be a crucial issue to understanding the physical properties of changing-look active galactic nucleus (CL-AGN). Here, we present the results of an intensive and homogeneous 6-month long reverberation mapping (RM) monitoring campaign during a low-activity state of the CL-AGN Seyfert galaxy NGC 3516. Photometric and spectroscopic monitoring was carried out during 2018--2019 with the Lijiang 2.4 m telescope. The sampling is 2 days in most nights, and the average sampling is $\sim$3 days. The rest frame time lags of H$\alpha$ and H$\beta$ are $\tau_{\rm{H}\alpha}=7.56^{+4.42}_{-2.10}$ days and $\tau_{\rm{H}\beta}=7.50^{+2.05}_{-0.77}$ days, respectively. From a RMS H$\beta$ line dispersion of $\sigma_{\rm{line}} = 1713.3 \pm 46.7$ $\rm{km}$ $\rm{s^{-1}}$ and a virial factor of $f_{\sigma}$ = 5.5, the central black hole mass of NGC 3516 is estimated to be $M_{\rm{BH}}= 2.4^{+0.7}_{-0.3} \times 10^{7} M_{\odot}$, which is in agreement with previous estimates. The velocity-resolved delays show that the time lags increase towards negative velocity for both H$\alpha$ and H$\beta$. The velocity-resolved RM of H$\alpha$ is done for the first time. These RM results are consistent with other observations before the spectral type change, indicating a basically constant BLR structure during the changing-look process. The CL model of changes of accretion rate seems to be favored by long-term H$\beta$ variability and RM observations of NGC 3516., Comment: 25 pages, 6 figures, Accepted for publication in ApJ

Context. Observations of young, low-mass, main-sequence, and zero-age main-sequence stars show evidence of a correlation between lithium abundance and chromospheric activity, albeit with a very large scatter. Fast rotation stars (including T Tauri stars, RS CVn, and BY Dra systems) show the Li I doublet at 6707.8 Å in their spectra. The lithium depletion is probably related to the rotation (turbulent diffusion induced by rotation). Because the flare activity of stars increases with decreasing rotation period, a correlation can be expected between lithium abundance and chromospheric activity for active stars. Aims. The aim of this paper is to investigate the relation between lithium abundance and the Ca II H and K emission index (R′HK = LHK/Lbol) for a sample of active stars. Methods. Based on the high-resolution spectroscopic observations, we calculated lithium abundance for 14 chromospherically active late-type stars using the comparison of the measured Li I λ670.8 nm equivalent width with curve of growth calculations in non-local-thermodynamic-equilibrium conditions. We also searched the correlation between lithium abundance and the Ca II H & K emission index (log R′HK) for the 14 chromospherically active late-type stars. Results. The study of the relationship between lithium abundance and the Ca II H & K emission index (log R′HK) found that the activity of sample stars increases with increasing lithium abundance. Next, the lithium abundance analogs progressively decrease as the rotation periods increase (rotation becomes slow) and the large values of the log R′HK along with small values of Rossby numbers for the sample of chromospherically active stars. Conclusions. The lithium abundance (log N(Li)) versus the chromospheric activity and log N(Li) against the rotation period both indicate that the lithium abundance analogs progressively increase as the chromospheric activity index increases and/or the rotation velocity increase (rotation period becomes small) for our sample of active stars. On the other hand, the log R′HK against the Rossby number RO shows that there is a clear trend of increasing activity with increasing rotation velocity for these active stars. Considering that the lithium abundance decreases with increasing stellar age in late-type stars, we can deduce that the chromospheric activity and the rotation velocity both decrease with the increase of stellar age for our sample active stars.

Lijiang 2.4-meter Telescope(LJT), the largest common-purpose optical telescope in China, has been applied to the world-wide astronomers since 2008. It is located at Gaomeigu site, Lijiang Observatory(LJO), the southwest of China. The site has very good observational conditions. Since 10-year operation, several instruments have been equipped on the LJT. Astronomers can perform both photometric and spectral observations. The main scientific goals of LJT include photometric and spectral evolution of supernova, reverberation mapping of active galactic nucleus, physical properties of binary star and near-earth object(comet and asteroid), identification of exoplanet, and all kinds of transients. Until now, the masses of 41 high accretion rate black holes have been measured, and more than 168 supernova have been identified by the LJT. More than 190 papers related to the LJT have been published. In this paper, the general observation condition of the Gaomeigu site is introduced at first. Then, the LJT structure is described in detail, including the optical, mechanical, motion and control system. The specification of all the instruments, and some detailed parameters of the YFOSC is also presented. Finally, some important scientific results and future expectations are summarized., Comment: 20 pages, 14 figures, accepted by Research in Astronomy and Astrophysics(RAA)

In order to study short timescale optical variability of $\gamma$-ray blazar S5 0716+714, quasi-simultaneous spectroscopic and multi-band photometric observations were performed from 2018 November to 2019 March with the 2.4 m optical telescope located at Lijiang Observatory of Yunnan Observatories. The observed spectra are well fitted with a power-law $F_{\lambda}=A\lambda ^{-\alpha}$ (spectral index $\alpha >0$). Correlations found between $\dot{\alpha}$, $\dot{A}$, $\dot{A}/A$, $\dot{F_{\rm{\lambda}}}$, and $\dot{F_{\rm{\lambda}}}/F_{\rm{\lambda}}$ are consistent with the trend of bluer-when-brighter (BWB). \textbf{The same case is for colors, magnitudes, color variation rates, and magnitude variation rates of photometric observations.} The variations of $\alpha$ lead those of $F_{\rm{\lambda}}$. Also, the color variations lead the magnitude variations. The observational data are mostly distributed in the I(+,+) and III(-,-) quadrants of coordinate system. Both of spectroscopic and photometric observations show BWB behaviors in S5 0716+714. The observed BWB may be explained by the shock-jet model, and its appearance may depend on the relative position of the observational frequency ranges with respect to the synchrotron peak frequencies, e.g., at the left of the peak frequencies. \textbf{Fractional variability amplitudes are $F_{\rm{var}}\sim 40\%$ for both of spectroscopic and photometric observations. Variations of $\alpha$ indicate variations of relativistic electron distribution producing the optical spectra. }, Comment: 28 pages, 11 figures, accepted in ApJ

Intelligent insecticidal lamp with LED is more efficient than ordinary insecticidal lamp. It used solar battery as the power supply, used high voltage power grid as hunting tools, used power LED which was controlled by singlechip as trapping tools for killing more insects. It could work at the night in spring or summer by data acquisition of clock chip and sensors and could automatically shut down in the rainy day or foggy day.

We present high-resolution spectroscopic observations for a sample of 21 young, solar-type stars near the Sun recently discovered in the X-ray wavelength range during the ROSAT all-sky survey. Based on these observations, we derive the lithium (Li) abundances of these 21 sample stars. Using the lithium abundances and the X-ray luminosity, we investigated the relationship between the Li abundances and the X-ray activity. We found a clear correlation between the lithium abundances and the X-ray luminosity: as the X-ray luminosity became stronger, the lithium abundance decreases in our sample stars. Our sample results provide further evidence that a correlation appears to exist between Li abundances, X-ray activity and age for a large number of solar-type stars. The results also confirm the presence of very active young stars close to the Sun, in agreement with recent findings from UV and X-ray surveys.

We present high-resolution spectroscopic observations for a sample of 19 weak-line T Tauri stars (WTTSs). Based on these observations and data of 108 WTTSs taken from the literature, we derive lithium abundances for 127 WTTSs. Investigation of a possible relation between lithium and rotation in WTTSs shows that: (1) rapidly rotating WTTSs have comparatively lower lithium abundances than their slower rotating counterparts; (2) in the spectral-type range G0-K0, most of the WTTSs share the same Li content irrespective of their T eff; and (3) active late-type binaries do not obey the correlation between lithium abundances and rotation periods, since the tidally locked rotation of the late-type binary system leads naturally to slower lithium destruction rates.

We monitored 16 X-ray selected young solar-type stars for light variation and found appreciable periodic light variability with amplitudes of a few hundredths of a magnitude in nine of the objects. Using the method of Phase Dispersion Minimization (PDM) and Fourier analysis (software PERIOD04), the rotation periods of these stars were determined from the photometric data. The rotation periods of all nine stars are shorter than about 3 days. It is suggested that, as with the Pleiades cluster, small amplitude light variations are quite common among young solar-type stars with rotation periods around 3 days or less. This gives further evidence for the spin up of solar-type stars predicted by models of angular momentum evolution of pre-main sequence stars.

We monitored the light variations of 16 solar-type stars recently discovered in the X-ray wave-length range during the ROSAT all-sky survey. We find that 9 out of 16 stars showed appreciable light variability with amplitudes of a few hundredths of a magnitude. They are all proved to be in periodic variations. Using the methods of the phase dispersion minimization (PDM) and Fourier Analysis (PERIOD04), we derive the photometric periods for these stars. The rotational periods are found range from 0.471 to 17.31 days and the period of stars most (of 7 stars) being shorter than 3 days. Apart from binaries system, the results give further evidence for the spin up of solar-type stars as predicted by models of angular momentum evolution of pre-main sequence stars.

We monitored the light curves of 22 weak-line T Tauri stars (WTTSs) discovered among the X-ray sources in the field of the Taurus-Auriga clou d. For 12 of the 22 WTTSs photometric periodic variability is confirmed and their rot ational periods are determined using Phase Dispersion Minimization (PDM) and Fourier analysis. Most of them are found to have periods shorter than one day. This gives further evidence for the spin up of solar-type stars predicted by the models of angular momentum evolution of pre-main sequence stars.

To explore the therapeutic effects of arthroscopy for post-traumatic chronic wrist pain.From February 2007 to June 2010, 12 patients with post-traumatic chronic wrist pain treated with arthroscopy were reviewed. Among the patients, 9 patients were male and 3 patients were female, ranging in age from 19 to 47 years, with a mean of 35.6 years. After physical examinations or MR abnormal findings, all the patients underwent wrist arthroscopic examination and treatment. Eight patients with tear in the central area of the triangular fibrocartilage complex (TFCC) underwent endoscopic partial resection. Two patients with relaxation of inter-carpal ligament after injury underwent radiofrequency shrinkage. One patient with distal radioulnar joint instability was treated with Kirschner fixation through distal radius and ulna in the neutral forearm rotation after clean-up of wrist joint, and also fixed with long arm cast immobilization for 6 weeks. One patient with ulnar impaction syndrome was treated with wrist clean, border modeling of triangular cartilage plate, partial resection of distal ulna.All the patients were followed up with an average duration of 10 months. Modified Mayo wrist score were evaluated from preoperative mean of (51.67 +/- 15.27) ( 25 to 75 scores) to postoperative mean of (77.92 +/- 10.54) (65 to 95 scores). Eleven patients recovered to normal work.Arthroscopy is an effective method for patients with post-traumatic chronic wrist pain which can diagnosis and cure the injuries under arthroscopy.

Surface lithium abundance and rotation velocity can serve as powerful and mutually complementary diagnostics of interior structure of stars. So far, the processes responsible for the lithium depletion during pre-main sequence evolution are still poorly understood. We investigate whether a correlation exists between equivalent widths of Li (EW(Li)) and rotation period (P$_{rot}$) for Weak-line T Tauri stars (WTTSs). We find that rapidly rotating stars have lower EW(Li) and the fast burning of Li begins at the phase when star's P$_{rot}$ evolves towards 3 days among 0.9M$_\odot$ to 1.4M$_\odot$ WTTSs in Taurus-Auriga. Our results support the conclusion by Piau & Turch-Chi��ze about a model for lithium depletion with age of the star and by Bouvier et al. in relation to rotation evolution. The turn over of the curve for the correlation between EW(Li) and P$_{rot}$ is at the phase of Zero-Age Main Sequence (ZAMS). The EW(Li) decreases with decreasing P$_{rot}$ before the star reaches the ZAMS, while it decreases with increasing P$_{rot}$ (decreasing rotation velocity) for young low-mass main sequence stars. This result could be explained as an age effect of Li depletion and the rapid rotation does not inhibit Li destruction among low mass PMS stars., 5 figures

The China possesses more than 70% Ginkgo resources in the world. The purposes of this research are to collect fine seedling and grafting clones in China, to probe genetic law on flavone glycosides and terpenes on Ginkgo leaves, and select leaf-used cultivars of high-pharmaceutical composition. In this research, we have collected 87 clones from 13 provenances and have carried out randomized block experiment at Tancheng, Laizhou and Yaoxiang in Shandong Province. Flavone glycosides and terpenes were determined through HPLC method from an improved Van Beek (1991) techniques and Shimadzu Lc-10 AD (Japan). Data and breeding analyses were carried out through IBMPC and SPQG30 software. The results of variance analyses show that there are significant differences to flavone glycosides, terpenes in clones, and the law of genetic parameters on heritability (h2) and genetic variability coefficient (Gcv), is clonesexprovenance to flavone glycosides in ginkgo leaves. The sigma g2, h2, Gcv and delta G' in male tree clone leaves are higher than female clone leaves on flavone glycosides. We have found that there is a maximum flavone content clone among males and a maximum terpene clone among females. The results of Q-cluster analyses are consistent with R-factor analyses of twenty higher terpenes clones. The results of index selection show that the ri.Y2, E(I) and CGS' of multiple traits selection including (gamma) trait are higher than single trait and multiple traits selection excluding gamma. The direct or index selection is more suited to leaf-used cultivars of Ginkgo. The genetic stability of each clone was appraised by Wricke's ecovalence method and NassarHuhu noparameter method. Flavone glycosides and terpenes are more than 2.09%-2.57% and 0.33%-0.41%, respectively, and we have selected four clones.

Context. Lithium has long been recognized as a powerful tool for investigating the internal mixing of low-mass stars. In addition, accurate measurements of lithium abundances in young solar-type stars provide independent and reliable age diagnostics. Aims. To study the relationship between lithium and activity in normal solar type-type stars and determine the effectiveness of lithium and kinematics as activity indicators, we perform a lithium survey of nearby late-type stars. We search for nearby young solar-type stars and investigate the relationship between lithium abundances and X-ray activity by measuring logLx. Methods. On the basis of high-resolution spectroscopic observations, we derived the lithium abundances of 33 young solar-type stars by comparing the measured Li I λ 670.8 nm equivalent widths with the curve of growth calculations in non-LTE (NLTE) conditions. Results. We obtain the lithium abundances of a sample of young solar-type stars. Using the lithium abundance and X-ray luminosity, Lx, we investigate the relationship between Li abundance and X-ray activity. We find a clear correlation between lithium abundance (logN(Li)) and X-ray luminosity, log Lx, for our sample stars. Conclusions. As the X-ray luminosity, Lx, becomes stronger, the lithium abundance decreases in our sample (11 pre-main-sequence, 15 zero-age-main-sequence, and 7 young main-sequence) stars. The results imply that there is a large number of solar-type stars. A correlation appears to exist between Li abundance and age, thus confirming the presence of very active young stars close to the Sun.