A Chandra observation of the X-ray environment and jet of 3C 31

We have used a deep Chandra observation of the central regions of the twin-jet Fanaroff–Riley class I (FRI) radio galaxy 3C 31 to resolve the thermal X-ray emission in the central few kpc of the host galaxy, NGC 383, where the jets are thought to be decelerating rapidly. This allows us to make high-precision measurements of the density, temperature and pressure distributions in this region, and to show that the X-ray emitting gas in the centre of the galaxy has a cooling time of only  5×10⁷ yr  . In a companion paper, these measurements are used to place constraints on models of the jet dynamics.
A previously unknown one-sided X-ray jet in 3C 31, extending up to 8 arcsec from the nucleus, is detected and resolved. Its structure and steep X-ray spectrum are similar to those of X-ray jets known in other FRI sources, and we attribute the radiation to synchrotron emission from a high-energy population of electrons. In situ particle acceleration is required in the region of the jet where bulk deceleration is taking place.
We also present X-ray spectra and luminosities of the galaxies in the Arp 331 chain of which NGC 383 is a member. The spectrum and spatial properties of the nearby bright X-ray source 1E 0104+3153 are used to argue that the soft X-ray emission is mostly due to a foreground group of galaxies rather than to the background broad absorption-line quasar.     

Chandra observations of the X-ray jet in 3C 66B

Our Chandra observation of the FR I radio galaxy 3C 66B has resulted in the first detection of an X-ray counterpart to the previously known radio, infrared and optical jet. The X-ray jet is detected up to 7 arcsec from the core and has a steep X-ray spectrum, α ≈1.3±0.1 . The overall X-ray flux density and spectrum of the jet are consistent with a synchrotron origin for the X-ray emission. However, the inner knot in the jet has a higher ratio of X-ray to radio emission than the others. This suggests that either two distinct emission processes are present or differences in the acceleration mechanism are required; there may be a contribution to the emission from the inner knot from an inverse Compton process or it may be the site of an early strong shock in the jet. The peak of the brightest radio and X-ray knot is significantly closer to the nucleus in the X-ray than in the radio, which may suggest that the knots are privileged sites for high-energy particle acceleration. 3C 66B's jet is similar both in overall spectral shape and in structural detail to those in more nearby sources such as M87 and Centaurus A.     

The Doppler Effect and Spectral Energy Distribution of Blazars

The relativistic beaming model is adopted to discuss quantitatively the observational differences between radio-selected BL Lac objects (RBLs) and X-ray-selected BL Lac objects (XBLs), and between BL Lac objects and flat spectrum radio quasars (FSRQs). The main results are the following:(1) In the Doppler corrected color-color(αro^in-αox^in) diagram,XBLs and FSRQs occupy separated regions, while RBLs bridge the gap between them. These properties suggest that similar intrinsic physical processes operate in all the objects under a range of intrinsic physical conditions. (2) Our results are consistent with the results of Sambruna, Maraschi and Urry (1996) from other methods. We show the αxox introduced by Sambruna to be a good index for describing the energy distribution because it represents the intrinsic energy distribution and includes the Doppler correction. (3)The Doppler effect of relativistic beaming is the main mechanism, and the physical differences(such as magnetic fields, electron energies) are also important complementary factors for understanding the relation between XBLs and RBLS.     

Chemical evolution of the high redshift galaxies

We have tried to determine the rate of chemical evolution of high redshift galaxies from the observed redshift distribution of the heavy element absorption systems in the spectra of QSOs, taking into account the evolution in the intensity of the metagalactic UV ionizing radiation background, the radius and/or the co-moving number density of, and the fraction of mass in the form of gas in, the absorbers. The data for both the Lyman limit systems and the C IV systems have been fitted simultaneously. It seems that the abundance of carbon has possibly increased by about a factor of 5 to 20 from the cosmic time corresponding to the redshift ≃ 4 to 2. The data also suggest that either the radius or the co-moving number density of the galaxies increased with redshift up to z = 2.0 and decreased slowly thereafter. The total mass of the halo gas was higher in the past, almost equal to the entire mass of the galaxy at z = 4. The hydrogen column density distribution for Lyman limit systems predicted by the model is in agreement with the observed distribution.     

北京同步辐射装置准直测量控制网的设计与优化

在北京同步辐射装置升级改造中,为提高元件的安装精度,同时兼顾未来新增光束线的建设需要,在实验大厅建立了准直测量控制网,作为设备定位、调校、安装和变形监测等工作的基础。本文重点介绍该控制网的设计、优化与观测结果分析,特别阐述了激光精密测量技术的应用,以及对点位密度、测量精度及可靠性的控制。     

太湖北岸太阳辐射的影响因子研究

利用2007—2021年上海莘庄太阳能辐射仪（型号：EKO-MS6020）接收到的逐月最大太阳辐射（MSR）资料,以水平0°角辐射仪观测值为参考,分析了0°—25°不同仰角观测的MSR差异,评估了台站观测、欧洲中期天气预报中心（ECMWF）大气再分析（ERA5）资料与太阳能辐射仪观测辐射的差别。在此基础上,讨论了MSR与天气要素的关系及发生的环流背景和天气尺度演变特征。结果显示,上海莘庄的MSR季节波动范围为800—1300 W/m²,峰值和谷值分别出现在5月和12月。观测的最大MSR值接近太阳常数,年际变化幅度约200 W/m²。相对于0°角观测,当太阳能板倾角为5°—20°时,平均每个月MSR可多获得50—250 W/m²辐射,最佳倾角为20°。ERA5相对于观测MSR存在明显低估,年平均低估约200 W/m²。虽然两者的季节变化相关系数高达0.88,但是在空间和时间上存在显著差异,年际变化相关并不显著。针对与MSR时间相差小于3 d的大气环流背景合成,春、夏、秋、冬四季的环流结构存在差异,但总体来看,偏北风加强、云量偏少、温度偏高的天气过程有利于MSR出现。

     

基于光合有效辐射的西北太平洋柔鱼资源丰度和空间分布变动研究

光合有效辐射(PAR)对于海洋初级生产力具有显著的调控作用,会间接影响到头足类的资源丰度和渔场分布。本文根据2006−2015年上海海洋大学鱿钓科学技术组提供的柔鱼鱿钓数据和光合有效辐射卫星遥感数据,研究了光合有效辐射与西北太平洋柔鱼种群的关系,并评估了异常环境条件下光合有效辐射对柔鱼的影响。结果发现,柔鱼单位捕捞努力量渔获量(CPUE)、渔场纬度重心、PAR,及其空间分布均具有显著的月间变化。7−11月各月适宜PAR范围分别为36～39 E/(m²·d)、33～36 E/(m²·d)、24～27 E/(m²·d)、18 E/(m²·d)和12 E/(m²·d),最适宜PAR值分别为36 E/(m²·d)、33 E/(m²·d)、27 E/(m²·d)、18 E/(m²·d)和12 E/(m²·d)。此外,CPUE与PAR有显著正相关关系(p<0.05),且CPUE与各月适宜PAR范围占渔场比例也呈显著正相关(p<0.05);同时渔场纬度重心随各月最适PAR平均纬度变化而变化。在异常环境条件下,拉尼娜年份CPUE值比厄尔尼诺年份高,该年份PAR值异常增高可能是导致柔鱼资源丰度增加的因素之一。研究表明,光合有效辐射对于西北太平洋柔鱼资源丰度和空间分布具有显著影响。     

岩石破坏过程磁场效应实验研究及其对地震预报的意义

地震前岩石圈存在可观测的磁场前兆异常, 岩石破坏过程的磁场效应规律却鲜有研究.本文设计建立了岩石破坏磁场效应监测实验系统, 测试分析了岩石破坏过程磁场与载荷、声发射、电磁辐射之间的关系, 探讨了岩石破坏磁场产生机制与岩石破坏磁场效应对地震预报的意义.结果表明: 岩石在受载破坏过程能够产生磁场, 磁感应强度与载荷变化存在良好的对应关系.在受载前期, 磁感应强度波动增加, 受载中后期, 磁场强度显著增加; 主破坏发生时, 磁场强度快速增加并达到最大值.磁感应强度与累积声发射计数平均相关系数达到0.825, 呈高度相关, 表明磁场变化能够反映岩石的变形破坏阶段和状态.岩石破坏磁场的产生主要与电性变化有关, 运动电荷或电流的变化产生了磁场.岩石破坏磁场与电磁辐射同属于电磁信号, 磁场是一种极低频、连续、脉冲式的信号, 信号频率一般为0~20 Hz; 电磁辐射是一种瞬态、阵发性的电磁波, 信号频率一般为kHz~MHz.相对于电磁辐射, 磁场前兆异常先出现, 岩石破坏的磁场监测结果对于评估地震的临震预报具有显著的意义.

     

CT轴扫描和螺旋扫描模式对颅脑急诊患者影像质量与辐射剂量的影响

目的:探讨CT轴扫描和螺旋扫描模式对颅脑影像质量和辐射剂量的影响,为颅脑急诊CT患者合理选择扫描模式提供依据。方法:20例患者,急诊CT扫描采用螺旋扫描模式,首次复查时采用轴扫描模式。管电压120kV,管电流290mA,球管转速0.8s,层厚5mm,间隔5mm,螺距0.969∶1,标准重建算法。测量脑灰质和脑白质CT值和背景噪声,计算SNR和CNR,并对图像噪声、颅底伪影、脑灰、白质对比显示情况进行主观评分,扫描后从CT剂量报告中调取辐射剂量值。两种扫描模式影像质量组间比较采用配对t检验和独立样本卡方检验。结果:轴扫描模式时脑灰、白质CT值分别为(38.02±2.23)HU和(27.01±1.72)HU,螺旋扫描时脑灰、白质CT值分别为(37.76±2.22)HU和(26.99±1.69)HU。CT轴扫描和螺旋扫描模式时,脑白质CT值、SNR和CNR差异没有统计学意义(P>0.05,t=0.045,0.119,0.502),图像噪声、颅底伪影、脑灰、白质对比显示主观评分结果没有统计学意义(P>0.05,χ²=3.142,0.0,3.159)。有效剂量在螺旋扫描模式时为66mSv,在轴扫描模式时为43mSv,但螺旋扫描模式扫描时间短,后处理重组图像对影像诊断有意义。结论:从影像质量和辐射剂量两方面考虑,对颅脑急诊患者CT检查时首选轴扫描模式,但对躁动不合作患者或体位不合作患者应选择螺旋扫描模式。