Two sets of CCD photometric observations for contact binary TU Boo were obtained in 2020 and 2021.Different from its asymmetric light curves published from the literature,our BVRcIc-band curves show that the heights o...Two sets of CCD photometric observations for contact binary TU Boo were obtained in 2020 and 2021.Different from its asymmetric light curves published from the literature,our BVRcIc-band curves show that the heights of maximum are almost equal.These distortions of light curves possibly indicate that the components were active in past 25 yr,but they were stable in the last two years.For total-eclipse binary TU Boo,due to some star-spots on the surface of the components,the physical structure obtained by many investigators are different.Therefore,the symmetric multi-color light curves in 2020,2021 are important for understanding configuration and evolution of this system.By using the Wilson–Devinney program,it is confirmed that TU Boo is an A-type shallow-contact binary with the temperature difference ofΔT=152 K and fill-out of f=14.67%.In the O−C diagram of orbital period analysis,a cyclic oscillation superimposed on a continuous decrease was determined.The long-term decreasing is often explained by the mass transfer from the more massive star to less massive one,this system will evolve into a deeper contact binary with time.The cyclic oscillations computed from much more CCD times of light minimum maybe result from the light-travel time effect via the presence of a third body.These characters of structure,evolution and ternary belong to typical A-type W UMa binaries with spectral G.展开更多
Summary： We performed a retrospective, case-control study to evaluate whether the urine flow acceleration （UFA, mL/s2） is superior to maximum uroflow （Qmax, mL/s） in diagnosing bladder outlet obstruction （BOO） ...Summary： We performed a retrospective, case-control study to evaluate whether the urine flow acceleration （UFA, mL/s2） is superior to maximum uroflow （Qmax, mL/s） in diagnosing bladder outlet obstruction （BOO） in patients with benign prostatic hyperplasia （BPH）. In this study, a total of 50 men with BPH （age： 58±12.5 years） and 50 controls （age： 59±13.0 years） were included. A pressure-flow study was used to determine the presence of BOO according to the recommendations of Incontinence Control Society （ICS）. The results showed that the UFA and Qmax in BPH group were much lower than those in the control group [（2.05±0.85） vs. （4.60±1.25） mL/s2 and （8.50±1.05） vs. （13.00±3.35） mL/s] （P〈0.001）. Accol;ding to the criteria （UFA〈2.05 mL/s2, Qmax〈10 mL/s）, the sensitivity and specificity of UFA vs. Qmax in diagnosing BOO were 88%, 75% vs. 81%, 63%. UFA vs. Omax, when compared with the results of P-Q chart （the kappa values in corresponding analysis）, was 0.55 vs. 0.35. The pros- tate volume, post void residual and detrusor pressure at Qmax between the two groups were 28.6±9.8 vs. 24.2±7.6 mL, 60.4±1.4 vs. 21.3±2.5 mL and 56.6±8.3 vs. 21.7±6.1 cmHzO, respectively （P〈0.05）. It was concluded that the UFA is a useful urodynamic parameter, and is superior to Qmax in diagnosing BOO in patients with BPH.展开更多
We present a study on pulsations of the high-amplitudeδScuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory（XAO）and t...We present a study on pulsations of the high-amplitudeδScuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory（XAO）and the Xinglong 85-cm telescope of National Astronomical Observatories,Chinese Academy of Sciences（NAOC）.Fourier analysis of the light curves reveals the fundamental radial mode and its five harmonics,with the fourth and fifth being newly detected.Thirtynine new times of maximum light are determined from the light curves,and combined with those in the literature,we construct the O-C diagram,derive a new ephemeris and determine a new value for the updated period of 0.104091579（2）.In addition,the O-C diagram reveals an increasing rate of period change for YZ Boo.Theoretical models are calculated and constrained with the observationally determined parameters of YZ Boo.The mass and age of YZ Boo are hence derived as M=1.61±0.05 M_⊙ and age=（1.44±0.14）×10~9 yr,respectively.With both the frequency of the fundamental radial mode and the rate of period change,YZ Boo is located at the post main sequence stage.展开更多
基金sponsored by Natural Science Foundation of Xinjiang Uygur Autonomous Region (No.2022DO1A164)the Joint Research Found (No.U1831109)in Astronomy under cooperative agreement between the National Natural Science Foundation of China (NSFC)and Chinese Academy of Sciences (CAS)the Natural Science Foundation of Shandong Province (No.ZR2020QA048)。
文摘Two sets of CCD photometric observations for contact binary TU Boo were obtained in 2020 and 2021.Different from its asymmetric light curves published from the literature,our BVRcIc-band curves show that the heights of maximum are almost equal.These distortions of light curves possibly indicate that the components were active in past 25 yr,but they were stable in the last two years.For total-eclipse binary TU Boo,due to some star-spots on the surface of the components,the physical structure obtained by many investigators are different.Therefore,the symmetric multi-color light curves in 2020,2021 are important for understanding configuration and evolution of this system.By using the Wilson–Devinney program,it is confirmed that TU Boo is an A-type shallow-contact binary with the temperature difference ofΔT=152 K and fill-out of f=14.67%.In the O−C diagram of orbital period analysis,a cyclic oscillation superimposed on a continuous decrease was determined.The long-term decreasing is often explained by the mass transfer from the more massive star to less massive one,this system will evolve into a deeper contact binary with time.The cyclic oscillations computed from much more CCD times of light minimum maybe result from the light-travel time effect via the presence of a third body.These characters of structure,evolution and ternary belong to typical A-type W UMa binaries with spectral G.
文摘Summary： We performed a retrospective, case-control study to evaluate whether the urine flow acceleration （UFA, mL/s2） is superior to maximum uroflow （Qmax, mL/s） in diagnosing bladder outlet obstruction （BOO） in patients with benign prostatic hyperplasia （BPH）. In this study, a total of 50 men with BPH （age： 58±12.5 years） and 50 controls （age： 59±13.0 years） were included. A pressure-flow study was used to determine the presence of BOO according to the recommendations of Incontinence Control Society （ICS）. The results showed that the UFA and Qmax in BPH group were much lower than those in the control group [（2.05±0.85） vs. （4.60±1.25） mL/s2 and （8.50±1.05） vs. （13.00±3.35） mL/s] （P〈0.001）. Accol;ding to the criteria （UFA〈2.05 mL/s2, Qmax〈10 mL/s）, the sensitivity and specificity of UFA vs. Qmax in diagnosing BOO were 88%, 75% vs. 81%, 63%. UFA vs. Omax, when compared with the results of P-Q chart （the kappa values in corresponding analysis）, was 0.55 vs. 0.35. The pros- tate volume, post void residual and detrusor pressure at Qmax between the two groups were 28.6±9.8 vs. 24.2±7.6 mL, 60.4±1.4 vs. 21.3±2.5 mL and 56.6±8.3 vs. 21.7±6.1 cmHzO, respectively （P〈0.05）. It was concluded that the UFA is a useful urodynamic parameter, and is superior to Qmax in diagnosing BOO in patients with BPH.
基金support from the National Natural Science Foundation of China(NSFC,Grant No.11273051)partially supported by the Chinese Academy of Sciences(CAS) “Light of West China” program(2015-XBQN-A-02)+4 种基金supported by the Strategic Priority Research Program of CAS(Grant No.XDB23040100)support from the Joint Fund of Astronomy of NSFC and CAS(Grant U1231202 and 11673003)the National Basic Research Program of China(973 Program 2014CB845700 and 2013CB834900)the LAMOST FELLOWSHIP supported by Special Funding for Advanced Users,budgeted and administrated by the Center for Astronomical MegaScience,Chinese Academy of Sciences(CAMS)support from the NSFC(No.11403088)
文摘We present a study on pulsations of the high-amplitudeδScuti star YZ Boo based on photometric observations in Johnson V and R bands with both the Nanshan 1-m telescope of Xinjiang Astronomical Observatory（XAO）and the Xinglong 85-cm telescope of National Astronomical Observatories,Chinese Academy of Sciences（NAOC）.Fourier analysis of the light curves reveals the fundamental radial mode and its five harmonics,with the fourth and fifth being newly detected.Thirtynine new times of maximum light are determined from the light curves,and combined with those in the literature,we construct the O-C diagram,derive a new ephemeris and determine a new value for the updated period of 0.104091579（2）.In addition,the O-C diagram reveals an increasing rate of period change for YZ Boo.Theoretical models are calculated and constrained with the observationally determined parameters of YZ Boo.The mass and age of YZ Boo are hence derived as M=1.61±0.05 M_⊙ and age=（1.44±0.14）×10~9 yr,respectively.With both the frequency of the fundamental radial mode and the rate of period change,YZ Boo is located at the post main sequence stage.
