以《Southern Star》为例看澳大利亚社区报

澳大利亚社区报多为免费发行，只有少数社区报在便利店出售。布里斯班的社区报《SouthernStar》，每周二至周四会被用皮筋卷成卷扔到每家信箱边的草地上。

欢迎加入“粉丝公社”——走进《STAR》杂志,让你的美丽为你喜欢的明星添光加彩!

你对自己的形象有信心吗?你对你喜欢的电影、明星、歌手有什么心里话吗?你愿意成为本刊"粉丝公社"特别推荐的"明星会员"吗?以"展示自我观点,体现明星价值"为目的的"粉丝公社"自我推荐榜将为你提供一个展示自己风采的舞台。还在犹豫什么呢?赶快行动吧。《STAR》杂志"粉丝公社"

欢迎加入“粉丝公社”——走进《STAR》杂志,让你的美丽为你喜欢的明星添光加彩!

你对自己的形象有信心吗?你对你喜欢的电影、明星、歌手有什么心里话吗?你愿意成为本刊"粉丝公社"特别推荐的"明星会员"吗?以"展示自我观点,体现明星价值"为目的的"粉丝公社"自我推荐榜将为你提供一个展示自己风采的舞台。还在犹豫什么呢?赶快行动吧。《STAR》杂志"粉丝公社"栏目现面向大众火爆征集,只要你热情美丽、青春阳光,那么,来吧,"粉丝公社"的下一期人物就有你哟!

骨科机器人联合Starr骨盆复位架治疗Tile C型骨盆环骨折

目的:探讨骨科机器人联合Starr骨盆复位架治疗Tile C型骨盆环骨折的临床疗效。方法:2019年10月至2021年5月采用机器人联合Starr骨盆复位架治疗14例Tile C型骨盆环骨折患者,男9例,女5例;年龄33~69岁。14例患者均为新鲜闭合骨折且不合并股骨、胫腓骨骨折等损伤。入院后4~7 d完成手术,术中在可透视碳素床,通过Starr骨盆复位架牵引复位骨盆环,联合骨科机器人治疗C型骨盆环骨折。观察手术时间、出血量、单枚螺钉置入透视次数、骨折复位质量、患肢功能及并发症等。采用Matta评分标准进行放射学复位评价,末次随访采用Majeed骨盆功能评分系统进行临床疗效评价。结果:14例患者均顺利完成手术,手术时间84~141 min,手术出血量20~50 ml,单枚螺钉置入透视次数4~9次。14例患者均获得随访,随访时间12~24个月。术后所有骨折获得骨性愈合,愈合时间3~7个月,未发现内固定断裂、螺钉松动、感染、神经损伤等并发症。依据Matta影像学复位评估标准:优9例,良4例,可1例。末次随访采用Majeed骨盆功能评分系统:优10例,良4例。结论:机器人联合Starr骨盆复位架治疗C型骨盆环新鲜骨折操作简单、缩短了手术和麻醉时间、并发症少,降低了手术风险,实现了骨盆骨折的微创治疗。但对于陈旧性骨折,因骨折复位困难,该技术并不适用。对于螺钉进钉点区域粉碎的骨折,通道螺钉置入困难,建议采用其他方式固定。对于伴有骨盆外伤史或骨盆发育异常者,术前需仔细评估有无经皮螺钉通道,避免损伤神经、血管。

STAR基因与东湖杂交奶绵羊繁殖性状的关联分析

本实验旨在探究类固醇激素合成急性调节蛋白(Steroidogenic Acute Regulatory Protein,STAR)基因多态性与东湖杂一代奶绵羊发情鉴定评分、产羔数的相关性,鉴定出影响绵羊繁殖性能的关键性位点。本研究以339只东湖杂一代奶绵羊为研究对象,采用竞争性等位基因特异性PCR(KASP)技术对STAR基因的g.31959747T>C、g.31959875A>C2个位点进行基因分型,并利用GLM模型对SNP位点与发情鉴定评分和产羔数进行关联分析。结果表明,g.31959747T>C与奶绵羊发情鉴定评分呈极显著相关,TT型的发情表现更优,但与产羔数差异不显著;g.31959875A>C与发情评分和产羔数均无显著关系;聚合基因型与繁殖性状的关联分析结果表明,TCAC型个体在发情评分、平均产羔数方面均较低。综上,STAR基因g.31959747T>C位点是影响奶绵羊发情评分的关键性位点,可根据育种目标将g.31959747T>C位点作为提高奶绵羊同期发情效果的分子标记,同时将TCAC聚合基因型及时淘汰。本研究结果可为奶绵羊繁殖性状的选育提供参考。

日本沼虾StAR基因克隆及其低氧胁迫下表达分析

为了研究类固醇激素合成急性调节蛋白(steroidogenic acute regulatory protein, StAR)在日本沼虾应答低氧胁迫过程中所发挥的作用,实验应用c DNA末端快速扩增(RACE)PCR技术克隆了日本沼虾StAR全长cDNA序列,并利用在线软件对其序列特征进行生物信息学分析,采用半定量RT-PCR方法分析StAR在日本沼虾不同组织的分布情况,采用实时荧光定量PCR(qRT-PCR)与免疫印迹(Western blot)技术对其在不同低氧胁迫阶段中的表达规律进行检测,观察低氧胁迫下精巢组织中StAR蛋白免疫组化定位。结果显示,日本沼虾StAR其cDNA全长3 361 bp (NCBI登录号:MW263908),包括5′-UTR 323 bp,3′-UTR 2 129 bp,开放阅读框909 bp,编码302个氨基酸。氨基酸序列比对及系统进化分析结果显示,日本沼虾StAR基因与三疣梭子蟹等甲壳动物StAR聚类一支,具有最近的亲缘关系。半定量RT-PCR检测结果显示,StAR在日本沼虾不同组织中均有表达,其表达量在肝胰腺和心脏组织中最低,在精巢组织中表达处于较高水平。使用qRT-PCR技术检测日本沼虾精巢中StAR在低氧胁迫下时空表达情况,结果表明,与对照组相比,低氧处理组精巢中StAR基因表达量在1~48 h均显著上调,而在低氧处理组96 h显著降低。此外,本实验对StAR进行了原核表达及抗血清制备,采用Western blot检测StAR蛋白表达丰度基本与基因表达模式相似,免疫组化结果显示,StAR蛋白在精细胞与间质细胞中均有表达。综上所述,长期低氧胁迫显著降低了StAR基因的转录表达水平,并且该基因可能在类固醇合成路径及精子发生过程中均发挥重要作用。本研究结果为进一步解析日本沼虾类固醇激素合成分子机制奠定基础。

STAR基因在不同发育期绵羊睾丸和附睾中的表达与组织分布

为探讨STAR基因在发育的绵羊睾丸和附睾中的表达模式及潜在功能,该研究采集3月龄、 1周岁和3周岁藏绵羊睾丸和附睾(头、体和尾)组织样本,利用实时荧光定量PCR、蛋白免疫印迹和免疫组织荧光染色法检测STAR基因的表达及其编码蛋白的细胞定位。结果发现,随着年龄的增加,在藏绵羊睾丸和附睾(附睾头除外)中STAR基因在转录水平的表达总体呈下降趋势,而在蛋白质水平的表达呈上调趋势。STAR蛋白主要存在于藏绵羊睾丸间质细胞和附睾假复层纤毛上皮主细胞。鉴于间质细胞和主细胞的主要生物学功能是分泌睾酮和分泌促进精子成熟所需的蛋白质,由此推测,STAR基因可能主要在睾丸间质细胞和附睾主细胞的发育和功能维持中发挥作用,进而促进雄激素的合成和精子的成熟。

Free Energy of Anisotropic Strangeon Stars

Can pulsar-like compact objects release further huge free energy besides the kinematic energy of rotation?This is actually relevant to the equation of state of cold supra-nuclear matter,which is still under hot debate.Enormous energy is surely needed to understand various observations,such asγ-ray bursts,fast radio bursts and softγ-ray repeaters.In this paper,the elastic/gravitational free energy of solid strangeon stars is revisited for strangeon stars,with two anisotropic models to calculate in general relativity.It is found that huge free energy(>10^(46)erg)could be released via starquakes,given an extremely small anisotropy((p_(t)-p_(r))/p_(r)~10^(-4),with pt/pr the tangential/radial pressure),implying that pulsar-like stars could have great potential of free energy release without extremely strong magnetic fields in the solid strangeon star model.

基于压缩感知的STAR-RIS辅助毫米波系统信道估计

一种可同时透射和反射的可重构智能表面(simultaneously transmitting and reflecting reconfigurable intelligent surface,STAR-RIS)可以同时辅助位于其两侧用户的无线通信。针对STAR-RIS辅助下的双用户毫米波通信系统的上行链路信道估计问题进行了研究,并对两用户在角度域的联合稀疏特性进行了探究。基于级联信道的联合稀疏特性和压缩感知理论,将级联信道估计问题转化为稀疏信号恢复问题,并提出了一种位置判决正交匹配追踪(position-judgment orthogonal matching pursuit,PJ-OMP)算法以减少导频开销。仿真结果显示,与传统的正交匹配追踪(orthogonal matching pursuit,OMP)算法相比,所提出的算法能够减少信道估计的导频开销,即使在某一侧用户所分配的能量较少时也能够准确地估计信道。

靶向小鼠Star基因的CRISPR/Cas9系统构建与打靶效力评价

目的利用CRISPR/Cas9系统对小鼠Star基因进行精确编辑,构建模拟人类STAR基因突变的细胞模型。方法选择中国先天性类脂质性肾上腺皮质增生症(CLAH)患者的热点突变区域,并设计相应的单导向RNA(sgRNA)。构建表达sgRNA的重组质粒,将其与慢病毒包装质粒共同转染至HEK-293T细胞并制备慢病毒颗粒以感染小鼠TCMK细胞。采用嘌呤霉素进行病毒感染后阳性细胞的筛选,提取阳性细胞的基因组DNA,通过聚合酶链式反应(PCR)扩增目标位点的基因组DNA片段,并利用TA克隆和Sanger测序技术,对编辑位点与效率进行统计分析。结果成功设计了有效的sgRNA序列,并利用CRISPR/Cas9系统成功构建了编辑小鼠Star基因的细胞模型。结论本研究通过精确编辑小鼠Star基因,成功构建了模拟人类STAR基因突变的CRISPR/Cas9系统,为深入研究CLAH的致病机制及探索潜在治疗方法提供有力工具,具有重要的科学意义和应用价值。

STAR-RIS辅助多载波通信感知一体化系统的资源优化

针对频谱资源短缺和传统的智能反射面无法实现全空间覆盖的问题,研究了同时透射和反射的可重构智能表面(simultaneously transmitting and reflecting reconfigurable intelligent surface, STAR-RIS)辅助通信感知一体化系统。通过分配功率和子载波资源并优化STAR-RIS系数矩阵,使得在保证感知功能的前提下,最大化通信和速率。设计了一种交替优化算法,将多变量之间相互耦合的非凸问题解耦转化为3个凸的子问题。首先,松弛子载波选择变量后使用惩罚函数和逐次凸逼近算法;然后,直接求解功率分配变量的凸子问题;最后,使用半正定规划并把秩一约束改写为核范数与谱范数之差,将其作为惩罚函数,使用逐次凸逼近以优化STAR-RIS系数矩阵。仿真结果表明,与传统RIS相比,所提方案的性能取得了显著提升。

基于改进A-star算法的轮椅无障碍出行路径规划策略研究

随着当前城市出行空间环境的复杂化,针对轮椅无障碍出行路径规划问题,文章提出一种基于改进A-star算法的轮椅无障碍出行路径规划策略。首先分析轮椅出行路径的影响因素,通过结合出行障碍以及出行时间两种影响因素将出行地图进行栅格化处理,同时将出行障碍函数融入A-star算法的成本函数中,实现对A-star算法的改进。最后通过实例进行仿真验证,结果表明:改进后的A-star算法可以有效地考虑轮椅出行障碍,并规划出合适的轮椅出行路径,验证了文章所提出策略的有效性。

Spectroscopic Observations of Ten Galactic Wolf-Rayet Stars at Bosscha Observatory:Determination of Stellar Parameters and Mass-loss Rates

We present optical spectra of 10 Galactic Wolf-Rayet(WR)stars that consist of five WN and five WC stars.The optical observation was conducted using a low-resolution spectrograph NEO-R1000(λ/Δλ~1000)at GAO-ITB RTS(27.94 cm,F/10.0),Bosscha Observatory,Lembang.We implemented stellar atmosphere Postdam Wolf-Rayet(PoWR)grid modeling to derive stellar parameters.The normalized optical spectrum can be used to find the best model from the available PoWR grid,then we could derive stellar temperature and transformation radius.To derive luminosity,stellar radius and color excess,we conducted a Spectral Energy Distribution(SED)analysis with additional data on the near-ultraviolet spectrum from the International Ultraviolet Explorer(IUE)database,and UBV and 2MASS JHK broadband filter data.Additional analysis to derive asymptotic terminal wind velocity was conducted from the P-Cygni profile analysis of the high-resolution IUE ultraviolet spectrum.With previously derived parameters,we could determine the mass loss rate of the WR stars.Furthermore,we compared our results with previous work that used PoWR code and the differences are not more than 20%.We conclude that the PoWR spectral grid is sufficient to derive WR stellar parameters quickly and could provide more accurate initial parameter input to the PoWR program code.

Formation of a Rapidly Rotating Classical Be-star in a Massive Close Binary System

This paper investigates the spin-up of a mass-accreting star in a close binary system passing through the first stage of mass exchange in the Hertzsprung gap. Inside an accreting star, angular momentum is carried by meridional circulation and shear turbulence. The circulation carries part of the angular momentum of the accreted layers to the accretor's surface. The greater the rate of arrival of angular momentum in the accretor is, the greater this part. It is assumed that this part of the angular momentum can be removed by the disk further from the accretor. If the angular momentum in the matter entering the accretor is more than half the Keplerian value, then the angular momentum obtained by the accretor during mass exchange stage does not depend on the rate of arrival of angular momentum. The accretor may have the characteristics of a Be-star immediately after the end of mass exchange.

Rotating Massive Strangeon Stars and X-Ray Plateau of Short GRBs

Strangeon stars,which are proposed to describe the nature of pulsar-like compact stars,have passed various observational tests.The maximum mass of a non-rotating strangeon star could be high,which implies that the remnants of binary strangeon star mergers could even be long-lived massive strangeon stars.We study rigidly rotating strangeon stars in the slowly rotating approximation,using the Lennard-Jones model for the equation of state.Rotation can significantly increase the maximum mass of strangeon stars with unchanged baryon numbers,enlarging the mass-range of long-lived strangeon stars.During spin-down after merger,the decrease of radius of the remnant will lead to the release of gravitational energy.Taking into account the efficiency of converting the gravitational energy luminosity to the observed X-ray luminosity,we find that the gravitational energy could provide an alternative energy source for the plateau emission of X-ray afterglow.The fitting results of X-ray plateau emission of some short gamma-ray bursts suggest that the magnetic dipole field strength of the remnants can be much smaller than that of expected when the plateau emission is powered only by spin-down luminosity of magnetars.

Analysis of the Impact of the Blazhko Effect Both on the Van Hoof Effect and Radial Velocity Amplitude in the Star RR Lyr

The Van Hoof effect is a phase shift existing between the radial velocity curves of hydrogen and metallic lines within the atmosphere of pulsating stars.In this article,we present a study of this phenomenon through the spectra of the brightest pulsating star RR Lyr of RR Lyrae stars recorded for 22 yr.We based ourselves,on the one hand,on 1268 spectra(41 nights of observation)recorded between the years 1994 and 1997 at the Observatory of Haute Provence(OHP,France)previously observed by Chadid and Gillet,and on the other hand on 1569 spectra(46nights of observation)recorded at our Oukaimeden Observatory(Morocco)between 2015 and 2016.Through this study,we have detected information on atmospheric dynamics that had not previously been detected.Indeed,the Van Hoof effect which results in a clear correlation between the radial velocities of hydrogen and those of the metallic lines has been observed and analyzed at different Blazhko phases.A correlation between the radial velocities of different metallic lines located in the lower atmosphere has been observed as well.For the first time,we were able to show that the amplitude of the radial velocity curves deduced from the lines of hydrogen and that of FeⅡ(λ4923.921?)increases toward the minimum of the Blazhko cycle and decreases toward the maximum of the same Blazhko cycle.Furthermore,we found that the Van Hoof effect is also modulated by the Blazhko effect.Thus,toward the minimum of the Blazhko cycle the Van Hoof effect is more visible and at the maximum of the Blazhko cycle,this effect is minimal.We also observed the temporal evolution of the amplitudes of the radial velocities of the lower and upper atmosphere.When observed over a long time,we can interpret it as a function of the Blazhko phases.

Close Major-merger Pairs at z=0: Star-forming Galaxies with Pseudobulges

We present a study of star-forming galaxies (SFGs) with pseudobulges (bulges with Sérsic index n<2) in a loca close major-merger galaxy pair sample (H-KPAIR).With data from new aperture photometries in the optical and near-infrared bands (aperture size of 7 kpc) and from the literature,we find that the mean Age of central stellar populations in Spirals with pseudobulges is consistent with that of disky galaxies and is nearly constant against the bulge-to-total ratio (B/T).Paired Spirals have a slightly lower fraction of pure disk galaxies (B/T≤0.1) than their counterparts in the control sample.Compared to SFGs with classical bulges,those with pseudobulges have a higher (>2σ) mean of specific star formation rate (sSFR) enhancement (sSFR_(enh)=0.33±0.07 versus sSFR_(enh)=0.12±0.06) and broader scatter (by~1 dex).The eight SFGs that have the highest sSFR_(enh)in the sample all have pseudobulges.A majority (69%) of paired SFGs with strong enhancement (having sSFR more than5 times the median of the control galaxies) have pseudobulges.The Spitzer data show that the pseudobulges in these galaxies are tightly linked to nuclear/circum-nuclear starbursts.Pseudobulge SFGs in S+S and in S+E pairs have significantly (>3σ) different sSFR enhancement,with the means of sSFR_(enh)=0.45±0.08 and-0.04±0.11respectively.We find a decrease in the sSFR enhancements with the density of the environment for SFGs with pseudobulges.Since a high fraction (5/11) of pseudobulge SFGs in S+E pairs are in rich groups/clusters (loca density N_(1Mpc)≥7),the dense environment might be the cause for their low s SFR_(enh).

An Asymmetric Galactic Stellar Disk Traced by OB-type Stars from LAMOST DR7

Using 9943 OB-type stars from LAMOST DR7 in the solar neighborhood,we fit the vertical stellar density profile with the model including a single exponential distribution at different positions(R,Φ).The distributions of the scale heights and scale length show that the young disk traced by the OB-type stars is not axisymmetric.The scale length decreases versus the azimuthal angleΦ,i.e.,from.■kpc withΦ=-3°to■kpc withΦ=9°.Meanwhile we find signal of non-symmetry in the distribution of the scale height of the north and south of the disk plane.The scale height in the north side shows signal of flaring of the disk,while that of the south disk stays almost constant around h_(s)=130 pc.The distribution of the displaceeent of the disk plane Z_(0)also shows variance versus the azimuthal angleΦ,which displays significant differences with the warp model constrained by the Cepheid stars.We also test different values for the position of the Sun,and the distance between the Sun and the Galactic center affects the scale heights and the displacement of the disk significantly,but that does not change our conclusion that the disk is not axisymmetric.

On the Identification of N-rich Metal-poor Field Stars with Future Chinese Space Station Telescope

During the long term evolution of globular clusters(GCs), some member stars are lost to the field. The recently found nitrogen-rich(N-rich) metal-poor field stars are promising candidates of these GC escapees, since N enhancement is the fingerprint of chemically enhanced populations in GCs. In this work, we discuss the possibility of identifying N-rich metal-poor field stars with the upcoming Chinese Space Station Telescope(CSST). We focus on the main survey camera with NUV, u, g, r, i, z, y filters and slitless spectrograph with a resolution about 200.The combination of UV sensitive equipment and prominent N-related molecular lines in the UV band bodes well for the identification: the color–color diagram of(u-g) versus(g-r) is capable of separating N-rich field stars from normal halo stars, if metallicity can be estimated without using the information on u-band photometry.Besides, the synthetic spectra show that a signal-to-noise ratio of 10 is sufficient to identify N-rich field stars. In the near future, a large sample of N-rich field stars found by CSST, combined with state-of-the-art N-body simulations will be crucial to deciphering GC-Galaxy co-evolution.

The ALMA-QUARKS Survey.Ⅱ.The ACA 1.3 mm Continuum Source Catalog and the Assembly of Dense Gas in Massive Star-Forming Clumps

Leveraging the high resolution,sensitivity,and wide frequency coverage of the Atacama Large Millimeter/submillimeter Array(ALMA),the QUARKS survey,standing for“Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures”,is observing 139 massive starforming clumps at ALMA Band 6(λ~1.3 mm).This paper introduces the Atacama Compact Array(ACA)7 m data of the QUARKS survey,describing the ACA observations and data reduction.Combining multiwavelength data,we provide the first edition of QUARKS atlas,offering insights into the multiscale and multiphase interstellar medium in high-mass star formation.The ACA 1.3 mm catalog includes 207 continuum sources that are called ACA sources.Their gas kinetic temperatures are estimated using three formaldehyde transitions with a non-LTE radiation transfer model,and the mass and density are derived from a dust emission model.The ACA sources are massive(16–84 percentile values of 6–160 M_(⊙)),gravity-dominated(M∝R^(1.1))fragments within massive clumps,with supersonic turbulence(M>1)and embedded star-forming protoclusters.We find a linear correlation between the masses of the fragments and the massive clumps,with a ratio of 6%between the two.When considering fragments as representative of dense gas,the ratio indicates a dense gas fraction(DGF)of 6%,although with a wide scatter ranging from 1%to 10%.If we consider the QUARKS massive clumps to be what is observed at various scales,then the size-independent DGF indicates a self-similar fragmentation or collapsing mode in protocluster formation.With the ACA data over four orders of magnitude of luminosity-to-mass ratio(L/M),we find that the DGF increases significantly with L/M,which indicates clump evolutionary stage.We observed a limited fragmentation at the subclump scale,which can be explained by a dynamic global collapse process.