Polarization observations of the radio cores of AGN — I. A sample of quasars     

D. J. Saikia  G. F. Holmes  A. R. Kulkarni  C. J. Salter  & S. T. Garrington 《Monthly notices of the Royal Astronomical Society》1998,298(3):877-887

We present total-intensity and linear-polarization observations at a single epoch for a sample of 11 quasars and one BL Lac object. The data were taken with the VLA A array at λλ 20, 18, 6 and 2 cm. We examine the variation of the degree of polarization, p , and polarization position angle, PA, with wavelength, and attempt to determine the rotation measure, RM, of the cores in these sources. The degree of polarization does not exhibit any systematic variation with wavelength, the median values ranging from 2.3 to 3.5 per cent at the different wavelengths. The variation of PA with λ² is not linear over the entire wavelength range. However, for most sources the λλ 20-, 18- and 6-cm PAs do follow such a linear relationship, yielding a median |RM| of about 15 rad m⁻². In contrast, the λλ 6- and 2-cm observations give a median |RM| of about 129 rad m⁻². The long-wavelength emission is likely to originate from a spatially different part of the milliarcsec-scale jet from the λ 2-cm emission, which could turn over at a higher frequency and is likely to be more compact and located closer to the quasar nucleus. We have attempted to obtain linear fits over the entire wavelength range allowing for n  π ambiguities in the PAs, but the fits are not statistically significant. The low values of RM for these core-dominated sources suggest that either the radio emission from the jet intercepts few of the emission-line clouds and their confining medium, or the clouds have a small filling factor and are possibly magnetically confined.  相似文献   

A Polarization Study of Radio Galaxies and Quasars selected from the Molonglo Complete Sample     

C. H. Ishwara-Chandra  D. J. Saikia  V. K. Kapahi  & P. J. McCarthy 《Monthly notices of the Royal Astronomical Society》1998,300(1):269-286

We present total intensity and linear polarization observations made with the Very Large Array at λλ20 and 6 cm of a representative sample of 42 radio galaxies and quasars selected from the Molonglo complete sample. The sources have been chosen to be of large size to probe the depolarizing medium on these scales using our present data and later with observations at lower frequencies with the Giant Metrewave Radio Telescope. The λ20 and 6 cm data are of similar resolutions and show that depolarization between these two wavelengths is seen largely only in those lobes which are within about 300 kpc of the parent galaxy. Examination of the depolarization of the lobes with arm-length asymmetry shows that depolarization is observed predominantly for the lobe which is closer to the nucleus. There is also a trend for the lobe closer to the nucleus to be brighter, consistent with the scenario that the nearer lobe is interacting with a denser environment which is responsible for the higher depolarization and greater dissipation of energy. We have also examined the depolarization asymmetry of the lobes on opposite sides of the nucleus for galaxies and quasars. This shows that the depolarization asymmetry for quasars is marginally higher than that for galaxies. The depolarization properties of our sample are possibly determined by an asymmetric environment as well as the effects of orientation.  相似文献   

γ-ray burst ultraviolet/optical afterglow polarimetry as a probe of quantum gravity     

Yi-Zhong Fan †  Da-Ming Wei  Dong Xu 《Monthly notices of the Royal Astronomical Society》2007,376(4):1857-1860

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Constraining the geometry of the neutron star RX J1856.5−3754     

Wynn C. G. Ho 《Monthly notices of the Royal Astronomical Society》2007,380(1):71-77

RX J1856.5−3754 is one of the brightest, nearby isolated neutron stars (NSs), and considerable observational resources have been devoted to its study. In previous work, we found that our latest models of a magnetic, hydrogen atmosphere match well the entire spectrum, from X-rays to optical (with best-fitting NS radius   R ≈ 14  km, gravitational redshift   z _g∼ 0.2  , and magnetic field   B ≈ 4 × 10¹²  G). A remaining puzzle is the non-detection of rotational modulation of the X-ray emission, despite extensive searches. The situation changed recently with XMM–Newton observations that uncovered 7-s pulsations at the     level. By comparing the predictions of our model (which includes simple dipolar-like surface distributions of magnetic field and temperature) with the observed brightness variations, we are able to constrain the geometry of RX J1856.5−3754, with one angle <6° and the other angle     , though the solutions are not definitive, given the observational and model uncertainties. These angles indicate a close alignment between the rotation and the magnetic axes or between the rotation axis and the observer. We discuss our results in the context of RX J1856.5−3754 being a normal radio pulsar and a candidate for observation by future X-ray polarization missions such as Constellation-X or XEUS .  相似文献   

Probability distribution functions for the Sun's magnetic field     

J.O. Stenflo 《Astronomische Nachrichten》2010,331(6):585-588

Magnetoconvection structures the Sun's magnetic field cover a vast range of scales, down to the magnetic diffusion scale that is orders of magnitude smaller than the resolution of current telescopes. The statistical properties of this structuring are governed by probability density functions (PDFs) for the flux densities and by the angular distribution functions for the orientations of the field vectors. The magnetic structuring on sub‐pixel scales greatly affects the field properties averaged over the resolution element due to the non‐linear relation between polarization and magnetic field. Here we use a Hinode SOT/SP data set for the quiet Sun disk center to explore the complex behavior of the 6301–6302 Å Stokes line profile system and identify the observables that allow us to determine the distribution functions in the most robust and least model dependent way. The angular distribution is found to be strongly peaked around the vertical direction for large flux densities but widens with decreasing flux density to become isotropic in the limit of zero flux density. The noise‐corrected PDFs for the vertical, horizontal, and total flux densities all have a narrowly peaked maximum at zero flux density that can be fitted with a stretched exponential, while the extended wings decline quadratically (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

双频激电法在云南新发地区的应用          下载免费PDF全文

艾斯卡尔  李华  杨剑 《沉积与特提斯地质》2010,30(4):104-108

经过在测区进行双频中梯测量,圈定了4个激电异常,综合测区岩石的电性、物性特征,对异常进行了推断和解释。根据所测量的视幅频率和视电阻率结果分析,双频激电法完适应于云南地形起伏较大的地区,并能取得良好的地质效果。  相似文献   

高速Ia型超新星的蓝色超出: 星周介质的尘埃散射          下载免费PDF全文

胡茂凯  王力帆  王晓锋 《天文学报》2023,64(2):13-22

Ia型超新星起源于碳氧白矮星在质量接近钱德拉塞卡极限时的热核爆炸,并被广泛地用作宇宙学距离的标准烛光.然而, Ia型超新星的前身星系统和爆炸机制还存在很多不明确的地方.近几十年来, Ia型超新星的星周环境得到了越来越多的关注.星周介质的空间分布性质为探究Ia型超新星的物理起源提供了重要线索.同时星周尘埃的散射会在Ia型超新星晚期的光变曲线、光谱和偏振等方面产生可观测效应.光谱上正常的Ia型超新星可以分成两类:喷射物速度正常和高速Ia型超新星.对比两者的光变曲线可以发现高速Ia型超新星在光极大后几个月内有明显颜色偏蓝的超出.该蓝色超出可以通过星周介质中的尘埃散射拟合得到.同时, Ia型超新星晚期光谱的拟合可以限制星周尘埃的颗粒大小等性质,晚期的偏振信号可以有效地限制星周尘埃的空间分布.拟合结果表明针对Ia型超新星晚期的多次图像偏振观测是揭示其星周尘埃环境特征的重要手段.  相似文献   

皖南云岭金矿地球物理找矿模型   总被引：1，自引：0，他引：1  

万芬  王光杰  杨晓勇  胡祥云  林方丽  张云霞 《地球科学与环境学报》2014,(1):185-192

皖南云岭金矿位于长江中下游多金属成矿带与华南成矿带之间,属于江南造山带上的一个热液脉型矿床。基于云岭金矿区域地质背景,在该区开展了岩石露头测定、岩石标本物性测定和地球物理学相关研究。运用地面高精度磁测法,识别本区主要控矿构造为NE向断裂带。根据激发极化法圈定高极化率异常区,并结合相应区域电阻率(可控源音频大地电磁法)和磁异常分布特征建立4种地球物理模型:低阻-高极化模型、高阻-高极化模型、高极化-磁异常过渡带模型和高极化-高磁异常模型。这4种地球物理模型建立在该区岩石物性与矿床成因基础之上,分别对应不同含矿模型:低阻-高极化模型对应接触带上硫铁矿成矿区;高阻-高极化模型对应含矿硅化带;高极化-磁异常过渡带模型对应围岩蚀变带;高极化-高磁异常模型对应岩浆侵入区。依据以上模型,可圈定NE向断裂带、断裂带西侧高阻硅化带及东侧蚀变岩体为找矿有利靶区。  相似文献   

2000年以来广东省经济极化时空演变   总被引：1，自引：0，他引：1  

谢正峰 《云南地理环境研究》2014,(3):51-55

选择崔-王指数、变异系数和空间自相关等3种方法,以地级市为基本评价单元,对2000年以来广东省的经济极化的时空演变进行了分析。研究表明：（1）广东省经济极化程度呈上升趋势;（2）2000以来,广东省极化现象明显,但是经济总量的极化现象大于人均经济总量;（3）广东省人均GDP和GDP的Moran＇s I均为正值且呈现增大趋势,经济空间集聚程度呈增大趋势,但是人均GDP的空间集聚程度大于GDP;（4）从局部空间自相关关系来看,广东省经济极化格局2000年以来处于稳定状态。  相似文献   

双偏振雷达差分传播相移的五种滤波方法对比分析     

魏庆  ;胡志群  ;刘黎平 《成都信息工程学院学报》2014,(6):596-602

为了对双线偏振雷达的差分传播相移ΦDP进行滤波降噪处理,提高双线偏振雷达识别粒子、估测降水的能力。通过对C波段双线偏振雷达差分传播相移分别采用滑动平均、中值滤波、FIR滤波、卡尔曼滤波和小波分析5种不同方法地介绍,利用中国气象科学研究院灾害天气国家重点实验室移动式C波段双线偏振雷达(POLC)2013年外场试验观测资料,对比分析了经5种方法处理后的差分传播相移ΦDP径向数据,及其分别在降水估测中应用的效果。结果表明:采用FIR滤波方法、卡尔曼滤波方法和小波分析方法对ΦDP径向数据进行处理的效果比传统的滑动平均和中值滤波方法好;其中小波分析处理的ΦDP径向数据波动最小,再经过变距离法拟合的KDP数据的负值能够得到最有效地抑制,最后应用到R(KDP)降水估测中的精度最高。  相似文献