光纤阵列太阳光学望远镜偏振分析器设计

给出了满足光纤阵列太阳光学望远镜(FASOT,Fibre Arrayed Solar Optical Telescope)观测目标的偏振分析器的理论设计.它具有以下特点:(1)具备偏振光学开关功能,使得高偏振测量成为可能;(2)在750nm宽度范围内,对各Stokes偏振参量都具有50%以上的理论偏振测量效率,且总的偏振测量效率高于86.6%.使得观测者在如此宽波长范围内可对多条磁敏谱线同时进行偏振测量;(3)根据所选光球和色球线侧重于对线偏振或圆偏振的测量;(4)对偏振元件的制作工艺以及安装误差等具有相当好的容忍度.以上特性使该偏振分析器成为高性能的偏振测量设备.     

2006年3月29日日全食白光日冕偏振测量

报告了在埃及赛路姆观测到的2006年3月29日日全食白光偏振测量的基本结果.我们使用的是一架便携式反射望远镜,焦距为640mm(F/D=8).在物镜前方安置可旋转线偏振片,每次旋转角度45°,终端为尼康数码相机.观测过程中,改变曝光时间并旋转偏振片,总共获取20张数码照片.文中讨论并呈现了介于 1.3 R⊙＜r ＜3.0 R⊙范围内的白光偏振方向和偏振度的大小分布.     

恒星射电耀发6cm波段偏振观测试验

利用新疆天文台南山基地25m射电望远镜在6cm波段对恒星V772 Her和βPer进行了偏振观测试验.通过数据处理和校准得到恒星的射电光变曲线.探测到V772 Her的射电耀发现象,耀发时的线偏振度约达30%,偏振位置角约4°;探测到βPer的缓变成份及叠加其上的快速耀发,βPer耀发时线偏振很弱.     

红外相机OASIS的偏振器设计

介绍为日本冈山天文台１．８８ｍ镜红外相机（ＯＡＳＩＳ）研制的红外偏振器．该偏振器与ＯＡＳＩＳ配备可实现～４．１′视场的近红外成像偏振观测．偏振器包括可旋转的消色差半波片和固定的致冷偏振片,通过旋转半波片对入射光的调制取得线偏振测量．实际观测给出ＪＨＫ波段的偏振效率分别为８６．３％、９７．０％和９７．５％．并给出了ＯＡＳＩＳ偏振观测与前人观测结果的比较     

四颗南天脉冲星在1560 MHz上的偏振观测

本文给出88年6月和7月期间在澳大利亚Parkes进行的一次南天脉冲星偏振观测的部分有意义的结果。频率为1560MHz。采用了Jodrell Bank天文台新研制成的2×16×5MHz滤波系统,使这次观测具有很强的消色散能力和较高的灵敏度。这4颗南天脉冲星具有较强的线偏振,为首次获得的高频偏振资料。     

ADS辅助实现线极化到圆极化的转换

给出C波段双圆极化低噪声接收机中圆极化输出的实现方案,研究了利用90°电桥进行线- 圆极化转换时两个线极化通道增益及相位的平衡度对圆极化隔离的影响。分析了如何通过调节一对同轴电缆的长度差来补偿相位不平衡,并借助ADS软件计算了该长度差,实现了线-圆极化转换,取得接收机两个圆极化之间的隔离度好于20dB的效果。     

分子云磁场与尘埃导致的偏振

磁场对分子云及其中的恒星的形成和演化起到重要的作用.分子云磁场的探测方法主要是谱线塞曼效应、尘埃热辐射的偏振,以及谱线的线偏振观测.利用谱线的塞曼效应可以直接测量视线方向的磁场强度.尘埃热辐射偏振可以有效地示踪磁场方向在天球上的分布.分子云内部的磁场会受到不同物理过程的影响.高分辨率观测可以研究磁场扰动的细节,低分辨率观测可以得到分子云甚至银河系大尺度磁场的宏观信息.只有多波段的观测才能全面地认识分子云磁场与各种物理过程的联系.该文对分子云尘埃热辐射偏振的观测情况做了调研,总结了分子云大尺度磁场的研究现状和发展前景.     

射电脉冲星的偏振特性与逆康普顿散射（ICS）模型

大量射电脉冲星的偏振观测－包括红偏振和圆偏振，个别脉冲的生直偏振模式，累积脉冲的消偏振现象等－为辐射区的物理状态和辐射提供了非常确切的观测事实，但现有理论对大从观测事实尚无法给出完整的说明，综述了脉冲星的偏振观测特征，并利用逆康谱顿散射模型对这些特性进行了解释。     

一九七五年天鹅座新星的偏振测光

对1975年天鹅座新星进行了偏振测光。没有发现可觉察的圆偏振。黄光波段新星的线偏振约为1.2%,蓝光波段约为1.1％。没有发现偏振的明显变化,偏振可能是属于星际起源的。     

基于斩波轮技术的K波段接收机噪声校准研究

接收机是射电天文中用于探测微弱射电信号的重要接收设备.接收机的强度校准就是将接收机对射电源的响应转换为天文意义上的流量密度.常规方法就是使用经典的冷热负载法,将接收机自身的强度响应转换为一个等效的温度值,之后再据此对射电源做进一步标定.通过搭建基于斩波轮技术的K波段接收机强度校准平台,使用斩波轮法测试K波段常温接收机的噪声温度,并与传统冷热负载法的测试结果进行比对.结果显示,在晴好天气条件下,斩波轮法在30°、90°仰角下噪声温度的最大测试误差为7.5%和8.4%,可以很好地应用于实际噪声温度测试中;但在5°仰角测试中,由于过低仰角引入了地面噪声,使得斩波轮法的测试误差上升至20%–30%之间而无法使用.希望在此基础上进一步开展K波段天空亮温度的理论计算与实测,从而完善斩波轮技术的应用,使之可以满足在不同气象条件下的噪声校准测试需求.     

Circular Polarization of Starlight

Of the 7500 stars cited in the Catalog of starlight polarization, those which satisfy the condition P _obs % and A _V 0^m.5 are selected. It is presumed that the selected stars (n=216) have circularly polarized light.     

耀变体在射电波段的偏振研究

利用UMRAO数据库22个耀变体源的偏振数据,根据Lazarian&Pogosyan理论模型分析研究了耀变体射电波段的偏振随波长的变化,得出不同类的耀变体偏振随波长变化的原因。结果表明,与Lazarian&Pogosyan理论模型吻合较好。由此得出如下结论:(1)反常去偏振耀变体源中反常法拉第旋光起主导作用,反常去偏振相对较少;(2)热辐射与同步辐射混合作用,高频波段的偏振度小于低频波段的偏振度(反常去偏振);(3)当被观测波段波长小于吸积盘热辐射对应的维恩波长时,高频波段的偏振度大于低频波段的偏振度(常规去偏振)。     

Polarization transfer in a pulsar magnetosphere

Propagation of radio waves in the ultrarelativistic magnetized electron–positron plasma of a pulsar magnetosphere is considered. The polarization state of the original natural waves is found to vary markedly on account of the wave mode coupling and cyclotron absorption. The change is most pronounced when the regions of mode coupling and cyclotron resonance approximately coincide. In cases when the wave mode coupling occurs above and below the resonance region, the resultant polarization appears essentially distinct. The main result of the paper is that in the former case the polarization modes become non-orthogonal. The analytical treatment of the equations of polarization transfer is accompanied by numerical calculations. The observational consequences of polarization evolution in pulsar plasma are discussed as well.     

Polarization measurements with an imaging gamma-ray telescope

The proposed Tracking and Imaging Gamma-Ray Experiment (TIGRE), operating in the 0.3–100 MeV energy interval, will be an efficient polarimeter with a modulation factor of 50% at 0.5 MeV. The polarization detection parameters of TIGRE were estimated using a Monte Carlo simulation modified to include the polarization dependence of the Klein-Nishina formula. Using Compton scattering of low energy photons and approximately 3 acceptance angle after scattering, TIGRE will be able to measure strong sources with 20% fractional polarization at 3 significance in a typical balloon-borne exposure and 5% during a 4-week satellite observation.     

Polarization in IR bands and the structure of cosmic dust grains

The water ice and silicate dust bands centered at about 3 and 10 μm, respectively, are simultaneously observed in the spectra of several objects. So far the wavelength dependence of the polarization in both bands has been modeled using two-layer spheroids, with the shape of the silicate core being confocal to that of the ice mantle. We show that nonconfocality of the spheroidal core and mantle boundaries changes fundamentally the wavelength dependence of the polarization within the 10-μm silicate band and affects significantly the polarization within the 3-μm water ice band, while the extinction profiles of these bands remain essentially unchanged. Since the results have been obtained for a theoretical model, we discuss their applicability and significance for cosmic dust grains. Original Russian Text ? M.S. Prokopjeva, V.B. Il’in, 2007, published in Pis’ma v Astronomicheskiĭ Zhurnal, 2007, Vol. 33, No. 10, pp. 784–791.     

Polarization observations of four southern pulsars at 1560 MHz

We present some interesting results from the mean pulse polarization observations of four southern pulsars made at the Australian National Radio Astronomy Observatory, Parkes, using the 64-m telescope in June and July, 1988. The 2 × 16 × 5 MHz filter system from Jodrell Bank has proved excellent in de-dispersing the pulse signals and measuring their polarization properties. We give the data for the four pulsars in some detail and discuss their spectral behaviour.     

Polarization of synchrotron emission from relativistic reconfinement shocks

We study the polarization properties of relativistic reconfinement shocks with chaotic magnetic fields. Using our hydrodynamical model of their structure, we calculate synthetic polarization maps, longitudinal polarization profiles and discuss the spatially averaged polarization degree as a function of jet half-opening angle  Θ _j   , jet Lorentz factor  Γ _j   and observer inclination angle to the jet axis  θ_obs  . We find that for  θ_obs≲Θ _j   the wave electric vectors are parallel in the vicinity of the structure ends and perpendicular in between, while for  θ_obs > Θ _j   the polarization can only be perpendicular. The spatially averaged polarization degree does not exceed 30 per cent. Parallel average polarization, with polarization degrees lower than 10 per cent, has been found for  θ_obs < Θ _j   under the condition  Γ _j Θ _j > 1  . As earlier works predicted the parallel polarization from relativistic conical shocks, we explain our results by discussing conical shocks with divergent upstream flow.     

Polarization of radiation from Supernova 2005cs and possible physical mechanisms of its generation

We present R-band polarimetry and photometry for Supernova 2005cs. The polarimetric observations were performed with the AZT-8 telescope at the Crimean Astrophysical Observatory (Ukraine) using the ST-7 photometer-polarimeter of the Sobolev Astronomical Institute. A record (for supernovae) linear polarization, p = 8%, was detected; the position angle underwent a jump by ?90° during the evolution of the supernova brightness. Possible generation mechanisms of the polarized radiation at the photospheric stage of evolution of the supernova are briefly analyzed.     

Polarization observations of 66 southern pulsars

Mean pulse profiles and polarization parameters at 435, 660 or 1500 MHz obtained using the ATNF Parkes radio telescope are presented for 66 southern pulsars. About half of these pulsars were discovered in the Parkes southern pulsar survey and most have no previously published polarization parameters. Where possible, beam impact parameters and inclination angles are computed assuming a circular beam geometry and the rotating-vector model. Implications of the results for models of the pulse emission mechanism are briefly discussed.     

Polarization evolution in strong magnetic fields

Extremely strong magnetic fields change the vacuum index of refraction. Although this polarization-dependent effect is small for typical neutron stars, it is large enough to decouple the polarization states of photons travelling within the field. The photon states evolve adiabatically and follow the changing magnetic field direction. The combination of a rotating magnetosphere and a frequency-dependent-state decoupling predicts polarization phase lags between different wavebands, if the emission process takes place well within the light cylinder. This QED effect may allow observations to distinguish between different pulsar-emission mechanisms and to reconstruct the structure of the magnetosphere.