MgO衬底NbN/AlN/NbN多层膜的制备

本文主要讨论磁控溅射设备制备的NbN/AlN/NbN三层结构的技术工艺,为制备All-NbN的 NbN/AlN/NbN SIS 隧道结作准备.我们在室温下利用直流磁控溅射工艺制备了单晶NbN薄膜,并对其超导电性做了初步的研究;又利用射频磁控溅射工艺制备了取向较好的AlN薄膜.我们利用磁控溅射方法制作NbN/AlN/NbN多层薄膜,然后对制备SIS隧道结进行了一些探索.     

Star Formation in Molecular Cloud Associated with IRAS 07028-1100

The first mapping observations in 12^CO J=2-1 and 12^CO J=1-0 lines were made towards molecular cloud associated with IRAS 07028-1100. The results show a mono-polar outflow (primarily blueshifted component) near IRAS 07028-1100, which suggests that star formation is occurring in this region. On the basis of the MSX (Midcourse Space Experiment) band-A image, molecular cloud core contours, NVSS data and IRAS data, we identify IRAS 07028-1100 as an embedded young intermediate-mass star. According to the 2MASS data, we suggest a sequential star formation in the infrared cluster associated with IRAS 07028-1100.     

300GHz超导SIS接收机系统的设计与构建

超导SIS(Superconductor-Insulator-Superconductor)混频技术是新兴的低噪声检测技术.其卓越的低噪声性能已使其成为毫米波和亚毫米波频段灵敏度最高的谱线接收设备,接收机的自动控制和稳定性有更高的要求,研制能够长期稳定工作的接收机有很重要的意义.本文主要讨论了我们自行研究设计工作在4K温度,准光学系统的毫米波超导SIS接收机的组成部件,根据我们制备的超导SIS隧道结器件的特性指标,计算设计了300GHz波段的超导接收机天线和结的集成芯片.     

Statistical analysis of Fe abundances gradients in the Galaxy

Using the high precision data of the proper motions and parallaxes from Hipparcos catalogue, we obtained the orbital parameters of 1302 stars in the Galaxy based on the mass distribution model provided by Allen and Santillón. Fe abundances of 1295 stars among our samples were analyzed. With the correlation analyses between [Fe/H] and orbital parameters, we obtained that the Fe gradient is - 0.057 ± 0.007 dex/kpc along the direction of the maximum galactocentric distance (hereafter DG_max) in the range of 8.5 kpc < DG_max < 17 kpc. We also got the result that the vertical gradient is steeper than the radial gradient. Furthermore, we divided the samples into two subgroups: giants and dwarfs; F, G and K stars; and then analyzed them respectively. Our results show that the gradient becomes flatter and flatter from giants to dwarfs, from F type to G and K type stars. We also divided the samples into disk and halo stars using maximum vertical distance Z_max = 1 kpc as the criterion and got the result that the abundances of the disk stars are much higher than that of the halo stars. Our work suggests the existence of the galactic gradient and supports those chemlcal evolution medels which show that the halo was formed before the disk at the early stage of the Galaxy.     

MgO(111)上NbN和AlN薄膜的生长研究

在制备NbN/AlN/NbN隧道结的工艺过程中,为了获得具有优质单晶结构的NbN薄膜,我们在MgO(111)基片上探索了直流溅射法制备NbN薄膜的生长工艺条件,XRD研究分析表明,我们获得了单晶结构良好的NbN薄膜;为了支持作为上电极的NbN薄膜的生长,也需要良好的AlN薄膜用作势垒层,我们采用射频磁控溅射设备和纯净的Al靶对AlN薄膜进行了制备研究.实验结果表明,所获得的AlN薄膜具有六方c-轴取向,并讨论了衬底和薄膜界面处可能的结构情况.     

Mutual recombination in slow Si^＋ ＋ H^- collisions

This paper studies the process of mutual neutralization of Si^＋ and H^- ions in slow collisions within the multichannel Landau-Zener model. All important ionic-covalent couplings in this collision system are included in the collision dynamics. The cross sections for population of specific final states of product Si atom are calculated in the CM energy range 0.05 e∨/u-5 ke∨/u. Both singlet and triplet states are considered. At collision energies below -10 e∨/u, the most populated singlet state is Si（3p4p, ^1S0）, while for energies above -150e∨/u it is the Si（3p, 4p, ^1P1） state. In the case of triplet states, the mixed 3p4p（^3S1 ＋^3P0） states are the most populated in the entire collision energy range investigated. The total cross section exhibits a broad maximum around 200 300e∨/u and for ECM ≤ 10e∨/u it monotonically increases with decreasing the collision energy, reaching a value of 8 × 10^-13 cm^2 at ECM = 0.05 e∨/u. The ion-pair formation process in Si（3p^2 ^3PJ）＋H（1s） collisions has also been considered and its cross section in the considered energy range is very small （smaller than 10^-20 cm^2 in the energy region below 1 ke∨/u）.     

Magnetic Fields in Active Late—Type Stars

The very high resolution and high signal-to-noise ratio spectra of ten x-ray selected stars are obtained by the NAOC Coude spectropraph.Magnetic field measurements of these stars have been performed using the profileaddition technique.The magnetic field strength and filling factor are obtained,and we find that there exist strong magnetic fields on very active stars.     

Rs标准测量系统的研究及其误差讨论

本文主要介绍了按照目前国际上制定的超导薄膜表面阻抗Rs标准测量方案（IEC／TC90）设计并制造的Rs标准测量系统，对实验过程中系统的细节作了改进，测试精度及可靠性作了分析，实验及结果证明该标准的可行性，同时说明了我们的测试系统符合国际超导薄膜表面阻抗Rs标准 测量的要求。     

银河系Fe丰度梯度分析

利用依巴谷星表提供的高精度自行、三角视差,在Allen和Santillan 1991年提出的银河系质量分布模型的基础上,得出了1302颗恒星在银河系势场中的运行轨道,并对其中的1295个样本进行了丰度分析.通过把这些恒星的Fe丰度与其轨道参数做相关分析,得出在银心距8.5 kpcmax<17 kpc的范围内,Fe丰度梯度为(-0.057±0.007) dex/kpc,且沿银盘法向梯度明显大于沿径向的梯度.在此基础上,对其中的巨星,矮星F, G, K型星又分别进行了统计分析,并把样本分为盘星、晕星两类对其丰度进行比较,结果表明：Fe元素丰度梯度从巨星到矮星、从F型星到K型星有逐渐减缓的趋势;盘星丰度明显高于晕星丰度.研究进一步证实银河系铁丰度梯度确实存在,支持了在银河系早期晕族恒星先于盘族恒星形成、厚盘恒星先于薄盘恒星形成的化学演化模型.     

LAMOST medium-resolution spectroscopic survey of binarity and exotic star (LAMOST-MRS-B): Observation strategy and target selection

LAMOST-MRS-B is one of the sub-surveys of LAMOST medium-resolution ($R\sim7500$) spectroscopic survey. It aims at studying the statistical properties (e.g., binary fraction, orbital period distribution, mass ratio distribution) of binary stars and exotic stars. We intend to observe about 30000 stars ($10 {\rm mag}\leq G < 14.5$ mag) with at least 10 visits in five years. We first planned to observe 25 plates around the galactic plane in 2018. Then the plates were reduced to 12 in 2019 because of the limitation of observation. At the same time, two new plates located at the high galactic latitude were added to explore binary properties influenced by the different environments. In this survey project, we set the identified exotic and low-metallicity stars with the highest observation priorities. For the rest of the selected stars, we gave the higher priority to the relatively brighter stars in order to obtain high quality spectra as many as possible. Spectra of 49129 stars have been obtained in LAMOST-MRS-B field and released in DR8, of which 28828 and 3375 stars have been visited more than twice and ten times with $\rm SNR \geq 10$, respectively. Most of the sources are B-, A-, and F-type stars with $\rm -0.6< [Fe/H] < 0.4 $ dex. We also obtain 347 identified variable and exotic stars and about 250 stars with $\rm [Fe/H] <-1$ dex. We measure radial velocities (RVs) by using 892233 spectra of the stars. The uncertainties of RV achieve about $1$ ${\rm km \cdot s^{-1}}$and $10$ ${\rm km \cdot s^{-1}}$ for 95% of late- and early-type stars, respectively. The datasets presented in this paper are available at http://www.doi.org/10.57760/sciencedb.j00113.00035.