Assessment of the Implementation of Energy Conservation Opportunities Arising from Energy Audits;A Study of Four-Star and Five-Star Hotels in Nairobi Kenya

This study assesses the implementation of energy conservation opportunities in four-star and five-star hotels in Nairobi. The Covid-19 pandemic had a significant impact on the Hospitality Industry. Currently, there is a growing inclination to furnish guests with superior and sustainable services in an energy-efficient and eco-friendly way. Comprehensive research was conducted from energy audits gathered from the establishments and contracted auditing companies, on top of this, hotel staff were given digital questionnaires. To add to the data, the researcher surveyed the hotels with engineering managers. The Energy Audits found that all 10 hotels had adopted Energy Conservation Opportunities (ECOs). After further analysis, the mean adoption rate of Energy Conservation Opportunities (ECOs) during the past three years was 55.83%, which was below the aim of 100%. According to studies, hotel staff manages energy to cut costs. The researcher found that hotels use up a lot of energy. However, they have conservation potential, depending on government policies, costs, ease of implementation, and management commitment to sustainable practices. Essentially, Energy Conservation Opportunities (ECOs) reduce energy expenditures and boost reliable revenues, especially during high energy prices and uncertainty.

超声介导瘤内注射99-star治疗肝癌实验病理研究

目的 观察人肝癌 smmc- 772 1裸小鼠模型经中药 99- star治疗的形态学变化。方法 99- star组 11只 ,酒精组 5只 ,生理盐水组 3只 ,分别于背部及肝等移植癌中注射 99- star、酒精和生理盐水等药液。结果 各组移植癌中均出现不同程度坏死 ,以生理盐水组最轻 ;坏死类型 ,注射酒精瘤细胞的蛋白变性呈脱水为特征 ,而 99- star致肿瘤坏死则固缩性和溶解性兼有且发现坏死区间质疏松 ,瘤细胞间距甚宽及有炎症反应。结论 99- star可作为

Pulsations of Three Rapidly Oscillating Ap Stars TIC 96315731,TIC72392575,and TIC 318007796

We analyze the frequencies of three known roAp stars,TIC 96315731,TIC 72392575,and TIC 318007796,using the light curves from the Transiting Exoplanet Survey Satellite.For TIC 96315731,the rotational and pulsational frequencies are 0.1498360 day^(-1)and 165.2609 day^(-1),respectively.In the case of TIC 72392575,the rotational frequency is 0.25551 day^(-1).We detect a quintuplet of pulsation frequencies with a center frequency of135.9233 day^(-1),along with two signals within the second pair of rotational sidelobes of the quintuplet separated by the rotation frequency.These two signals may correspond to the frequencies of a dipole mode.In TIC318007796,the rotational and pulsational frequencies are 0.2475021 day^(-1),192.73995 day^(-1),and196.33065 day^(-1),respectively.Based on the oblique pulsator model,we calculate the rotation inclination(i)and magnetic obliquity angle(b)for the stars,which provide the geometry of the pulsation modes.Combining the phases of the frequency quintuplets,the pulsation amplitude and phase modulation curves,and the results of spherical harmonic decomposition,we conclude that the pulsation modes of frequency quintuplets in TIC96315731,TIC 72392575,and TIC 318007796 correspond to distorted dipole mode,distorted quadrupole mode,and distorted dipole mode,respectively.

GRB 210323A:Signature of Long-lasting Lifetime of Supra-massive Magnetar as the Central Engine from the Merger of Binary Neutron Star

Theoretically,a supra-massive neutron star or magnetar may be formed after the merger of binary neutron stars.GRB210323A is a short-duration gamma-ray burst(GRB)with a duration of lasting~1 s.The light curve of the prompt emission of GRB 210323A shows a signal-peaked structure and a cutoff power-law model can adequately fit the spectra with E_p=1826±747.More interestingly,it has an extremely long-lasting plateau emission in the X-ray afterglow with a duration of~10^(4)s,and then follows a rapid decay with a decay slope~3.2.This temporal feature is challenging by invoking the external shock mode.In this paper,we suggest that the observed long-lasting X-ray plateau emission is caused by the energy injection of dipole radiation from supra-massive magnetar,and the abrupt decay following the longlasting X-ray plateau emission is explained by supra-massive magnetar collapsing into a black hole.It is the short GRB(SGRB)with the longest X-ray internal plateau emission powered by a supra-massive neutron star.If this is the case,one can estimate the physical parameters of a supra-massive magnetar,and compare with other SGRBs.We also discuss the possible gravitational-wave emission,which is powered by a supra-massive magnetar and its detectability,and the possible kilonova emission,which is powered by r-process and magnetar spin-down to compare with the observed data.

超声介导瘤内注射“99-star”治疗人肝癌smmc-7721裸鼠模型中Bcl-2蛋白表达

目的 研究人肝瘤 smmc- 772 1裸小鼠模型经中药“99- star”治疗后 Bcl- 2蛋白表达。方法 于裸小鼠背部和肝等移植癌中 ,1 1只注射“99- star”,5只注射酒精和 3只注射生理盐水 ,动物处死后应用免疫组化方法检测移植癌组织中 Bcl- 2蛋白表达。结果 对照组与各实验组移植癌和移植癌组织与药物注射引起肿瘤坏死的 Bcl- 2蛋白表达 ,在统计学上有显著差别。结论“99- star”可供 B超介导治疗肝癌的有效药物目的 研究人肝瘤 smmc- 772 1裸小鼠模型经中药“99- star”治疗后 Bcl- 2蛋白表达。方法 于裸小鼠背部和肝等移植癌中 ,1 1只注射“99- star”,5只注射酒精和 3只注射生理盐水 ,动物处死后应用免疫组化方法检测移植癌组织中 Bcl- 2蛋白表达。结果 对照组与各实验组移植癌和移植癌组织与药物注射引起肿瘤坏死的 Bcl- 2蛋白表达 ,在统计学上有显著差别。结论“99- star”可供

KIC 10417986:Spectroscopic Confirmation of the Nature of the Binary System with aδScuti Component

KIC 10417986 is a short orbital period(0.0737 day)ellipsoidal variable star with aδSct andγDor hybrid pulsation component discovered by Kepler.The ground-based spectroscopic observations were carried out in the winters of 2020 and 2021 to investigate the binary nature of this star.We derive the orbital parameters using the rvfit code with a result of K_(1)=29.7±1.5 km s^(-1),γ=-18.7±1.7 km s^(-1),and confirm an orbital period of 0.84495 day instead of the result given by Kepler.The atmospheric parameters of the primary are determined by the synthetic spectral fitting technique with the estimated values of T_(eff)=7411±187 K,log g=4.2±0.3 dex,[M/H]=0.08±0.09 dex and vsini=52±11 km s^(-1).KIC 10417986 is a circular orbit binary system.From the single-lined nature and mass function of the star,the derived orbital inclination is 26°±6°,and the mass of the secondary is 0.52_(-0.09)^(+0.18)M_(⊙),which should be a late-K to early-M type star.Fourteen frequencies are extracted from Kepler light curves,of which six independent frequencies in the high-frequency region are identified as the p-mode pulsations ofδSct star,and one independent frequency in the low-frequency region(f_(2)=1.3033 cd^(-1))is probably the rotational frequency due to the starspots rather than the ellipsoidal effect.

基于Android的选矿破碎生产线PLC测控系统

为解决选矿企业破碎生产线传统控制中出现的工人长时间现场操作对健康影响大、设备关联自动化程度低、出现故障不能快速诊断等缺点,提出设计与开发基于Android的PLC测控系统。首先概述了选矿企业破碎生产线的目前运行状况、Android与PLC各自特性及其在测控行业的优点,然后根据矿山企业选矿设备位置分散以及实时安全管理的要求设计出破碎生产线2-Star型网络拓扑结构,并给出了下星网络与上星网络中的具体设备传感器采集信号与连接接口方式等内容。进而重点论述了系统中需要设计的PLC软件、ICC软件、Android软件系统主要模块与流程图,并对它们涉及到的数字滤波、线性标度、故障诊断等关键算法进行了详细的介绍。实际开发应用表明:该系统极大地改善了工人的操作环境、提高了破碎设备运行的稳定性与安全性,尤其当出现故障后技术人员可以快速诊断并修复,很大程度上降低了选矿企业的设备运行维护成本。

Revise Thermal Winds of Remnant Neutron Stars in Gamma-Ray Bursts

It seems that the wealth of information revealed by the multi-messenger observations of the binary neutron star(NS)merger event,GW170817/GRB 170817A/kilonova AT2017gfo,places irreconcilable constraints to models of the prompt emission of this gamma-ray burst(GRB).The observed time delay between the merger of the two NSs and the trigger of the GRB and the thermal tail of the prompt emission can hardly be reproduced by these models simultaneously.We argue that the merger remnant should be an NS(last for,at least,a large fraction of 1 s),and that the difficulty can be alleviated by the delayed formation of the accretion disk due to the absorption of high-energy neutrinos emitted by the NS and the delayed emergence of effective viscosity in the disk.Further,we extend the consideration of the effect of the energy deposition of neutrinos emitted from the NS.If the NS is the central object of a GRB with a distance and duration similar to that of GRB 170817A,thermal emission of the thermal bubble inflated by the NS after the termination of accretion may be detectable.If our scenario is verified,it would be of interest to investigate the cooling of nascent NSs.

Timing and Single-pulse Study of Pulsar J1909+0122 Discovered by CRAFTS

We report the discovery of PSR J1909+0122 by the Five-hundred-meter Aperture Spherical Radio Telescope(FAST)as part of the Commensal Radio Astronomy FAST Survey.PSR J1909+0122 has a spin period of 1.257 s and a dispersion measure of 186.2 pc cm^(-3).The averaged pulse profile shows two distinct components.We performed a single-pulse study based on a one-hour observation at 1.25 GHz on 2021 August 23.We used a threshold of 5σ_(ep) to measure the nulling fraction(NF)as 63%±1.5%.The longitude-resolved fluctuation spectra and fast Fourier transform spectra of the binary sequences revealed the quasi-periodicity of nulling with a period of 30 rotation periods.We examined the reliability of the periodicity by comparing it to random noise injection.The NF,E,and modulation periodicity P_(M) of PSR J1909+0122 were compared with other periodic nulling pulsars,showing that the source of J1909+0122 has the second largest NF in the population.Long-term timing observations over six months were used to derive the phase-connected ephemeris of this pulsar.The measured P and P values disfavor dipolar geometry for polar gap models,and the prediction for a space-charge-limited flow model in the case of inverse Compton scattering is only just above the death line.In this work,PSR J1909+0122 has revealed possible correlations between nulling behavior and pulsar properties,which will help to shed light on the pulsar emission mechanism and its temporal evolution in future observations.

Variable Star Detection in the Field of Open Cluster NGC 188

This work presents the charge-coupled device(CCD)photometric survey of the old open cluster NGC 188.Timeseries V-band photometric observations were conducted for ten nights in 2017 January using the Nanshan Onemeter Wide-field Telescope to search for variable stars in the field of the cluster.A total of 25 variable stars,including one new variable star,were detected in the target field.Among the detected variables,16 are cluster member stars,and the others are identified as field stars.The periods,radial velocities,effective temperatures,and classifications of the detected variables are discussed in this work.Most of the stars’effective temperatures are between 4200 and 6600 K,indicating their spectral types are G or K.The newly discovered variable is probably a W UMa system.In this study,a known cluster variable star(V21=V0769 Cep)is classified as an EA-type variable star based on the presence of an 0.5 mag eclipse in its light curve.

Past and Future of a Type Ia Supernovae Progenitor Candidate HD 265435

As one of the most useful cosmological distance indicators,type Ia supernovae(SNe Ia)play an important role in the study of cosmology.However,the progenitors of SNe Ia are still uncertain.It has been suggested that carbonoxygen white dwarf(CO WD)+He subgiant systems could produce SNe Ia through the double-degenerate(DD)model,in which the He subgiant transfers He-rich matter to the primary CO WD and finally evolves to another CO WD.Recently,a CO WD+He star system(i.e.,HD 265435)has been discovered to be a new SNe Ia progenitor candidate based on the DD model.The orbital period of the system is about 0.0688 days,and the masses of the CO WD and the He star are 1.01±0.15 M_(⊙) and 0.63_(-0.12)^(+0.13)M_(⊙),respectively.In this work,we evolve a large number of primordial binaries to the formation of CO WD+He star systems and investigate the evolutionary history of HD265435.We find that HD 265435 may originate from a primordial binary that has a 5.18 M_(⊙) primary and a3.66 M_(⊙) secondary with an initial orbital period of 5200 days.The CO WD+He star system would be formed after the primordial binary experiences two common-envelope ejection processes.We also find that HD 265435 would evolve to a double WD system with a total mass of 1.58 M⊙after a stable mass-transfer process,and the double WD system would merge driven by gravitational wave radiation.We estimate that it would take about 76 Myr for HD 265435 to form an SN Ia.In addition,HD 265435 would be a potential target of space-based gravitational wave observatories(e.g.,LISA,Taiji and TianQin).

磁共振检测重型β-地中海贫血患者内分泌腺体铁过载的临床意义

目的联合肝脏、胰腺、垂体磁共振T2-star(MRI T2*)评估重型β-地中海贫血(β-TM)患者相关脏器铁过载的临床意义,分析去铁酮治疗前后的肝脏、胰腺、垂体MRI T2*变化的临床意义。方法选择长期(输血史≥1年,输血次数>10次)治疗β-TM患者中年龄≥10岁26例,其中男性7例,女性19例。2010年7月～2011年7月规律输血,仅口服去铁酮去铁治疗,治疗前、服用去铁酮满1年时分别赴香港威尔斯亲王医院进行胰腺MRI T2*(胰腺T2*)、肝脏MRI T2*(肝脏T2*)、垂体MRIT2*(垂体T2*)检测。结果服用去铁酮治疗前,肝脏铁浓度(LIC)(22.42±7.21)mg/g;服用去铁酮满1年时,肝脏LIC(21.46±7.69)mg/g。治疗前后肝脏、胰腺、垂体MRI T2*值[(1.48±1.23)ms vs(1.55±1.18)ms,(9.09±9.96)ms vs(9.51±13.00)ms,(9.74±4.46)ms vs(10.14±4.76)ms]比较,差异无明显统计学意义(P>0.05)。治疗前后肝脏与胰腺MRI T2*值均呈正相关(P<0.05);治疗前后LIC与胰腺T2*值均呈负相关(P<0.05)。肝脏与垂体、胰腺与垂体MRI T2*值治疗前后均不相关(P>0.05)。年龄与肝脏、胰腺及垂体的MRI T2*值无相关关系(P>0.05)。结论 MRI T2*可以作为评估β-TM患者胰腺、垂体铁负荷有效、安全的检测工具;可通过肝脏铁负荷来推测胰腺铁负荷,胰腺铁负荷与年龄无关;但肝脏负荷并不能作为垂体铁负荷的推测手段。去铁酮的临床疗效难以定论,有待进一步研究。

星图S_4的交叉数

研究网络拓扑结构图星图S4的交叉数问题.首先构造星图S4好的画法,得到了S4交叉数的上界,然后给出了S4交叉数下界的数学证明,最终得到S4的交叉数的精确值为8.同时给出了与其具有同构关系的图S4,3和图A4,3的交叉数.

炼化企业氢管网设计与集成优化技术应用研究

随着加氢处理深度不断增加,炼化企业氢气用量和氢气品质需求不断提高,氢气管网集成优化已成为炼化企业高效利用氢气资源,实现节能减排、降本增效的重要措施。介绍了氢气管网系统的构成与特点,分析了氢气管网与供氢单元、用氢单元、氢回收单元之间的相互关系,介绍了氢气管网集成优化研究的目标、原则、方法与技术。抚顺石油化工研究院研究开发了集成加氢反应动力学模型的氢气系统优化专业软件(H2-STAR),根据各用氢单元氢分压、流量、循环氢纯度等适宜参数,并采用夹点分析与多目标综合优化相结合的方法,完成氢源、氢阱的合理匹配与整个系统的集成优化设计。某炼油厂氢气管网优化改造项目的工业应用表明,利用H2-STAR技术开展炼化企业氢管网优化设计与研究,有助于以较少的投资实现氢气梯级利用、提高氢气利用率和经济效益的目标。

PS Vir:a short-period solar-like contact binary

We present multi-color photometric observations and a one-dimensional spectrum, acquired from March 2016 to May 2017, for the short-period eclipsing binary PS Vir, by using the 2.16-m, 85-cm and 60-cm telescopes at Xinglong station, which is administered by National Astronomical Observatories, Chinese Academy of Sciences. The spectral type was determined as G2V from the one-dimensional spectrum. The photometric solution was reduced from BVRc light curves. The results imply that PS Vir is a W-subtype contact binary with a mass ratio of q - 0.305（zk0.008） and a fill-out factor of f = 14.4（＋1.8）%. The orbital period may be undergoing a cyclic oscillation with an ampli-tude of A = 0.0027（~0.0001）d and a modulated period of 11.7（4-0.2） yr, which may result from the light-time effect due to a third body. The lower limit on mass for the assumed component is 0.12 Me. Moreover, the more massive component of PS Vir may be a bit more evolved star as determined from the mass-luminosity diagram.

Optical flare events on the RS Canum Venaticorum star UX Arietis

Based on long-term high-resolution spectroscopic observations obtained during five observing runs from 2001 to 2004, we study optical flare events and chromospheric activity variability of the very active RS CVn star UX Ari. By means of the spectral subtraction technique, several optical chromospheric activity indicators （including the He IDa, Na I D1, D2 doublet, Ha and Ca II IRT lines） covered in our echelle spectra were analyzed. Four large optical flare events were detected on UX Ari during our observations, which show prominent He I D3 line emission together with great enhancement in emission of the Ha and Ca II IRT lines and strong filled-in or emission reversal features in the Na ! D1, D2 doublet lines. The newly detected flares are much more energetic than previous discoveries, especially for the flare identified during the 2002 December observing run. Optical flare events on UX Ari are more likely to be observed around two quadratures of the system, except for our optical flares detected during the 2004 November observing run. Moreover, we have found rotational modulation of chromospheric activity in the Ha and Ca II IRT lines, which suggests the presence of chromospherically active longitudes over the surface of UX Ari. The change in chromospherically active longitudes among our observing runs, as well as the variation in chromospheric activity level from 2001 to 2004, indicates a long-term evolution of active regions.

First time-resolved CCD photometry and time-series analysis of NSV 13601

We present the first results of a time-resolved CCD photometric and time-series analysis of NSV 13601,a variable star in the constellation Pegasus.The 14′′Schmidt-Cassegrain telescope of Maharaja Krishnakumarsinhji Bhavnagar University(MKBU)was used for observations.Analysis was performed both in VStar and Period04 software,and their results were compared.The main results are as follows:From data analysis,its has period^77.784 d(MKBU data V)(VStar),~77.632 d(MKBU data Ic)(VStar),~77.058 d(MKBU data V)(Period04)and^49.560 d(MKBU data Ic)(Period04).Its V and I mean magnitudes for MKBU data are 12.203(V)and 11.292(I)mag respectively.We confirm it to be a variable star.

On the radiation problem of high mass stars

A massive star is defined as one with mass greater than - 8-10.M⊙. Central to the on-going debate on how these objects [massive stars] come into being is the so-called Radiation Problem. For nearly forty years, it has been argued that the radiation field emanating from massive stars is high enough to cause a global re- versal of direct radial in-fall of material onto the nascent star. We argue that only in the case of a non-spinning isolated star does the gravitational field of the nascent star overcome the radiation field. An isolated non-spinning star is a non-spinning star without any circumstellar material around it, and the gravitational field beyond its surface is described exactly by Newton＇s inverse square law. The supposed fact that massive stars have a gravitational field that is much stronger than their radiation field is drawn from the analysis of an isolated massive star. In this case the gravitational field is much stronger than the radiation field. This conclusion has been erroneously extended to the case of massive stars enshrouded in gas and dust. We find that, for the case of a non- spinning gravitating body where we take into consideration the circumstellar material, at ,- 8-10M⊙, the radiation field will not reverse the radial in-fall of matter, but rather a stalemate between the radiation and gravitational field will be achieved, i.e. the infall is halted but not reversed. This picture is very different from the common picture that is projected and accepted in the popular literature where at -8-10 M⊙, all the circumstellar material, from the surface of the star right up to the edge of the molec- ular core, is expected to be swept away by the radiation field. We argue that massive stars should be able to start their normal stellar processes if the molecular core from which they form has some rotation, because a rotating core exhibits an Azimuthally Symmetric Gravitational Field which causes there to be an accretion disk and along this equatorial disk. The radiation field cannot be much stronger than the gravitational field, hence this equatorial accretion disk becomes the channel via which the nascent massive star accretes all of its material.

The first photometric investigations of the G-type shallow contact binary IO Cnc

IO Cnc was classified to be a new G-type(G0)W UMa-type eclipsing binary system.Our first multicolor photometric solutions show that IO Cnc is a new W-subtype shallow contact binary with a fill-out factor of f=16.1%and a low mass ratio of q=3.12(or 1/q=0.32).During orbital period investigations,a cyclic variation and a downward parabolic variation with a rate of(-1.28±0.43)×10^(-7) d yr^(-1) was discovered in the observed–calculated(O-C)curve.The cyclic variation was analyzed by the light travel time effect(LTTE)via a potential red dwarf companion star,an orbital semi-major axis shorter than 4.88±0.82 AU was obtained.Finally,we collect physical parameters of a sample of 50 G-type shallow contact binaries(f≤20%),it is suggested that most of the G-type shallow contact binaries are undergoing a longterm and periodic orbital period changes,especially more systems show long-term decreases.The long-term orbital period decrease indicates that IO Cnc is in a mass transferring from the more massive component to the less massive one.With the long-term decrease of the orbital period,this shallow contact binary will evolve into a deeper contact one.

Precise determination of fundamental parameters of six exoplanet host stars and their planets

The aim of this paper is to determinate the fundamental parameters of six exoplanet host （EH） stars and their planets. Because techniques for detecting exo- planets yield properties of the planet only as a function of the properties of the host star, we must accurately determine the parameters of the EH stars first. For this rea- son, we constructed a grid of stellar models including diffusion and rotation-induced extra-mixing with given ranges of input parameters （i.e. mass, metallicity and initial rotation rate）. In addition to the commonly used observational constraints such as the effective temperature Tell, luminosity L and metallicity [Fe/H], we added two obser- vational constraints, the lithium abundance log N （Li） and the rotational period Prot. These two additional observed parameters can set further constraints on the model due to their correlations with mass, age and other stellar properties. Hence, our estimations of the fundamental parameters for these EH stars and their planets have a higher preci- sion than previous works. Therefore, the combination of rotational period and lithium helps us to obtain more accurate parameters for stars, leading to an improvement in knowledge about the physical state of EH stars and their planets.