RUI: Radio Studies of the Interstellar Medium and Pulsars

RUI：星际介质和脉冲星的射电研究

• 批准号: 9530710
• 负责人: Joel Weisberg
• 金额: $ 14.37万
• 依托单位: Carleton College
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 1996
• 资助国家: 美国
• 起止时间: 1996-06-01 至 2001-05-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=9530710&HistoricalAwards=false
• 关键词: RUI; Radio; Studies; Interstellar; Medium

Weisberg AST-9530710 Radioastronomical studies of the interstellar medium and pulsars will be carried out. Observations will be conducted at the Arecibo Observatory in Puerto Rico, the Parkes radio telescope in Australia, the Green Bank Telescope in West Virginia, and the Very Large Array in New Mexico. In particular, the upgraded Arecibo Observatory telescope and the Green Bank Telescope will be highly sensitive instruments that will enable one to make much more sensitive observations than previously possible. The interstellar medium studies are divided into three main categories: In the first, neutral hydrogen line absorption spectra of distant pulsars will be obtained and measured and kinematic distances will be determined from these spectra. The electron densities along the pulsar-Earth lines of sight will then be derived from distances and dispersion measures, and models of the Galactic distribution of electrons will be compared with these results. In the second category, the spatial structure and physical properties of interstellar hydrogen will be studied with neutral hydrogen line absorption measurements of high- latitude and nearby pulsars and recombination line observations in the directions of pulsars. The third category consists of studies of the Galactic magnetic field through Faraday rotation measurements of polarized pulsar signals. Temporal and small- scale spatial variations will be studied in one experiment, while the broad structure of the magnetic field will be investigated in another. There are also three main categories of intrinsic pulsar investigations: First, full Stokes parameter pulsar polarization profiles will be measured and calibrated, and morphological classifications will be assigned on the basis of these and all other published observations. Second, polarized profiles will be examined for temporal variations that could indicate free precession or intrinsic beam changes as well as the Galactic magnetic field variations di scussed above. Third, the emission beam geometry will be studied via empirical/geometrical analyses and fits of the rotating vector model to measured position angles. Undergraduate students at Carleton College will be involved in the research program.

将进行星际培养基和脉冲星的Weisberg AST-9530710放射量研究。观察将在波多黎各的Arecibo天文台，澳大利亚的Parkes射程望远镜，西弗吉尼亚州的绿色银行望远镜以及新墨西哥州的大型阵列进行观察。特别是，升级的Arecibo天文台望远镜和绿色银行望远镜将是高度敏感的工具，使人们能够比以前更敏感。 星际培养基研究分为三个主要类别：在第一个中，将获得遥远脉冲星的中性氢系吸收光谱并测量，并从这些光谱中确定运动距离。然后，沿脉冲星 - 地球线的电子密度将来自距离和色散度量，将电子的银河分布模型与这些结果进行比较。在第二类中，将研究星际氢的空间结构和物理特性，并在高纬度和附近脉冲星的中性氢线吸收测量和脉冲星指示中的重组线观测。第三类包括通过极化脉冲星信号的法拉第旋转测量的银河磁场的研究。将在一个实验中研究时间和小规模的空间变化，而磁场的宽结构将在另一个实验中进行研究。 固有的脉冲星研究也有三个主要类别：首先，将测量和校准完整的Stokes参数Pulsar偏振轮廓，并根据这些和所有其他已发表的观察结果分配形态分类。其次，将检查极化轮廓的时间变化，这些变化可能表明自由进动或内在光束变化以及上面扫描的银河磁场变化。第三，将通过经验/几何分析和旋转矢量模型的拟合到测量位置角度来研究发射光束几何形状。 卡尔顿学院的本科生将参与研究计划。