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 be...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).According 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 prostate 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 cmH 2 O,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 the...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
Photometric results of three δ Scuti stars, AD Ari, IP Vir and YZ Boo from new observations obtained at the:Xinglong Station of the Beijing Astronom- ical Observatory (BAO) during 2000 aELd 2001 are reported. We pres...Photometric results of three δ Scuti stars, AD Ari, IP Vir and YZ Boo from new observations obtained at the:Xinglong Station of the Beijing Astronom- ical Observatory (BAO) during 2000 aELd 2001 are reported. We present here the preliminary analyses. Detailed studies of these stars based on additional data will be published separately.展开更多
Various times of light minima of the contact binary CK Boo are compiled and the correspnoding O C curve is analyzed with Kalimeris at al.’s method (1994). It is shown that the orbital period varies in a quasi sinusoi...Various times of light minima of the contact binary CK Boo are compiled and the correspnoding O C curve is analyzed with Kalimeris at al.’s method (1994). It is shown that the orbital period varies in a quasi sinusoidal form with a period of about 14 years and an amplitude of 0.26 × 10 -5 days while it undergoes a secular period increase dP/dE =+4 97 × 10 -7 days/year. The mechanisms that could explain the changes in the orbital period are also discussed.展开更多
文摘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).According 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 prostate 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 cmH 2 O,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.
文摘Photometric results of three δ Scuti stars, AD Ari, IP Vir and YZ Boo from new observations obtained at the:Xinglong Station of the Beijing Astronom- ical Observatory (BAO) during 2000 aELd 2001 are reported. We present here the preliminary analyses. Detailed studies of these stars based on additional data will be published separately.
文摘Various times of light minima of the contact binary CK Boo are compiled and the correspnoding O C curve is analyzed with Kalimeris at al.’s method (1994). It is shown that the orbital period varies in a quasi sinusoidal form with a period of about 14 years and an amplitude of 0.26 × 10 -5 days while it undergoes a secular period increase dP/dE =+4 97 × 10 -7 days/year. The mechanisms that could explain the changes in the orbital period are also discussed.
