视超光速源的统计分析

本文收集了视超光速源样本的有关观测数据，在同步加速自康普顿散射机制下导出了各源的多普勒因子，再利用视超光速源的相对论射束模型计算样本源的有关物理量，如射电光度和亮温度，并与它们的观测值作直接的比较，得到较好的相关结果。这些结果支持了活动星系核中具有相对论射束运动的假设。同时我们比较了样本源的射电、光学、Ｘ射线的发现它们之间有一定的相关性，说明在不同波段上的辐射机制可能存在某种联系。     

束－等离子体不稳定性直接放大电磁波及其对太阳Ⅲ型爆的解释

弱磁化相对论电子束注入等离子体时，由非共振波粒相互作用激发的束－等离子体不稳定性可以直接放大电磁波，计算结果表明：在偏离共振条件的区域，电磁波仍可在较宽的频率范围被放大，并在每个共振峰下形成平台结构。随着谐波数的增高，增长率峰值逐渐变小，峰宽也变窄。本文还分析了电磁波的增长率随背景参数ω＿（ｐｅ）／Ω＿ｅ及高能电子的入射方向和辐射方向的变化规律，在典型的日冕条件下，此类不稳定性所放大的电磁波的增长率大小、带宽、方向性、偏振及谐波等性质，可以用来解释太阳Ⅲ型射电爆发现象，本文的研究亦可用来解释其他天体等离子体辐射。     

Flux monitoring at 327 MHz during SL9-Jupiter collision

Jupiter flux at 327 MHz was monitored using the Ooty radio telescope from July 12th to July 29th during the collision of comet Shoemaker-Levi 9 with Jupiter. Flux was found to increase steadily from July 17th to July 26th by ∼ 2–5 Jy, after which it declined to its pre-event value. The comparison of 327 MHz observations with those at 840 MHz and 2240 MHz indicates that the enhancement was mainly due to the increased synchrotron emission and the contribution of thermal emission was very small at metric-decimetric frequencies. The enhancement in radio emission was found to be more at 840 MHz than at 327 or 2240 MHz. The steepening of the spectrum between 327 and 840 MHz as well as between 2240 and 840 MHz was also noted.     

Dense Gas, Chemistry and Star Formation in Luminous Galaxies

The molecular phase of the ISM constitutes the main source of fuel for the activity in starburst and AGNs. The physical conditions and chemical constitution of the molecular gas will change with, and respond to, the evolution of the activity. This paper includes a short discussion of the ¹²CO/¹³CO 1–0 line intensity ratio as a diagnostic tool of the molecular gas properties of luminous galaxies – paired with examples of high-resolution studies of how the line ratio varies within galaxies. A possible connection between the OH megamasers and galaxies with unusually high ¹²CO/¹³CO 1–0 line intensity ratios are also briefly discussed.The relative intensities of the dense gas tracers HNC, HCN, HCO⁺ and CN are a result of both chemistry and starburst evolution. The discussion on the interpretation of HNC 1–0 emission includes the importance of ion-neutral chemistry in a luminous starburst region. Finally, simple cartoon ISM models and how they can be applied to LIRGs and ULIRGs, are presented.     

Rapid reversals of polarization in spikes and fast fine structures

We briefly describe the polarization state of the spike groups and fast fine structures superimposed on the 47GB microwave burst of 1991 May 16. At two frequencies 100 MHz apart, namely, 2645 and 2545 MHz, the polarization showed rapid reversals on short time scales of the order of 50 100ms. We think this is probably related to fluctuations on both short time and small spatial scales, in the plasma density and magnetic field of the emission region. Thése oscillations cause the plasma and cyclotron frequency ratio to vary around the value of , thus making the electron cyclotron maser instability growth rate to be dominated alternately by the X mode and the O mode and the polarization state to switch from one sign to the other.     

The 18-cm light curves of the luminous radio supernova candidates in Arp 220

We present multi-epoch observations of Arp 220 with the VLBA and focus on the continuum emission from the luminous radio supernovae (RSNe) whose 1.6-GHz light curves are shown. The supernovae seem to be generally stable or only slowly decaying in flux with time, a result which deviates from the model of Type IIn RSNe. Hints of new eruptions confirm that they are indeed new sources and not supernova remnants, which could be several hundred years old. The slow decay of the sources for which monitoring data were available forces us to reconsider the starburst model for Arp 220 and adopt a more modest value of 0.7 yr⁻¹ for the supernova rate based on these new eruptions. The starburst efficiency should also be modified accordingly which gives rise to the issue of an active nucleus once more. The question is raised whether it is the starburst which creates this active nucleus, something which could affect the evolution of starburst galaxies as a group.     

The Spatial and Temporal Variability of Global Stratospheric Gravity Waves and Their Activity during Sudden Stratospheric Warming Revealed by COSMIC Measurements

This study investigates the spatial and temporal variability of global stratospheric gravity waves (GWs) and the characteristics of GW activity during sudden stratospheric warming (SSW) using the GPS radio occultation measurements from the COSMIC mission during September 2006 to May 2013. Corresponding to the COSMIC RO observational window and analysis method, GW potential energy (Ep) with vertical scales no shorter than ～2 km is resolved. It is found that the distributions of GW Ep over 20-30 km and 30-38 km show similar spatial and seasonal variations. The variations of GW Ep with altitude and latitude along the westerly wind are identified in different seasons over 60°-80°W. In the middle and high latitudes, seasonal cycles are distinct in the time-latitude and time-altitude distributions of GW activities, which show larger Ep in winters when westerly wind dominates and smaller Ep in summers when easterly wind dominates. The influence of quasi-biennial oscillation on GW activity is recognized in the tropics. GW Ep enhances closely following the occurrence of minor SSW events; while during major events, GW Ep may not enhance, and sometimes may even weaken, in the regions where reversals of zonal wind occur, probably caused by the filtering impact of the 0 m s-1 wind level on the GWs.     

对流层经验模型在中国VLBI站上的优化分析

利用2010~2012年的IGS天顶对流层延迟(ZTD)序列、ERA5格网数据积分ZTD序列,在中国4个VLBI站点上对目前常用的经验模型进行优化,分别建立Local_ERA和Local_ZTD模型。基于2013~2014年IGS并址站点ZTD数据,将改进后的2种模型与全球GPT2w模型、SHAO-Gm模型进行对比。结果表明,改进后的Local_ERA、Local_ZTD模型精度相近,相对于GPT2w、SHAO-Gm模型平均精度在4个VLBI站点上都有提高,尤其在水汽季节性变化较强的北京站改进效果明显;其中Local_ERA平均精度略高于Local_ZTD,比GPT2w模型精度提高7.90%,比SHAO-Gm模型精度提高21.26%。     

顾及季节性变化的日本区域加权平均温度建模

利用2014~2018年的ERA-Interim数据建立适用于日本区域的加权平均温度模型,分析其误差并进行季节性改正。结果表明：1）建立的线性加权平均温度模型精度比Bevis模型提高约16%;2）线性模型的残差时间序列存在季节性变化,因此对模型进行季节性改正,改正后的模型精度比Bevis模型和线性模型提高约37%和25%;3）将3种模型与探空站积分Tm进行比较,进一步说明季节性改正后模型的优越性。