High Resoultion Studies of Solar Flares, Active Regions, Prominences and the Quiet Sun at Centimeter and Millemeter Wavelengths

文章摘要：ATM99-09809建议标题：高分辨率研究太阳耀斑、活动区、日冕和厘米和毫米波长处的平静太阳首席研究员：马里兰大学Mukul R.Kundu研究人员将解决太阳物理中的基本问题，包括高能粒子的加速，活动区及其上方的磁场结构，以及大型日冕结构中的温度分布和能量学。这项工作与康普顿伽马射线天文台、Yokoh X射线卫星和太阳和日球层天文台(SOHO)上的EIT仪器的航天器观测密切相关，也与几个来源的矢量磁图测量密切相关。主要工作是获取和分析正确解释这些伽马、X射线、紫外线和光学数据所需的同步无线电测量数据。这些数据将主要从国家射电天文台的甚大阵列(VLA)、伯克利-伊利诺伊-马里兰毫米波阵列(BIMA)、日本的Nobeama射电日光仪和加利福尼亚州的欧文斯谷太阳能阵列获得。在目前的太阳活动高峰期的观测是该计划的一个特别重点。正确解释的无线电数据可以确定许多物理参数，如日冕磁场强度和活动区上方的磁配置，这些参数是任何其他技术无法获得的。对这些参数的了解对于任何太阳耀斑和活动区的模型都是至关重要的。

Abstract: ATM 99-09809Proposal Title: High Resolution Studies of Solar Flares, Active Regions, Prominences, and the Quiet Sun at Centimeter and Millimeter WavelengthsPrincipal Investigator: Mukul R. Kundu, University of MarylandThe investigators will attack fundamental problems in solar physics involving the acceleration of high-energy particles, the magnetic field structure in and above active regions, and the temperature distributions and energetics in large-scale coronal structures. The work is intimately associated with spacecraft observations from the Compton Gamma Ray Observatory, the Yokoh X-ray satellite, and the EIT instrument on the Solar and Heliospheric Observatory (SOHO), as well as vector magnetogram measurements from several sources. The main effort is to acquire and analyze simultaneous radio measurements necessary for proper interpretation of these gamma, X-ray, ultra-violet, and optical data. These data will be obtained primarily from the Very Large Array (VLA) of the National Radio Astronomy Observatory, the Berkeley-Illinois-Maryland Millimeter Array (BIMA), the Nobeyama Radioheliograph in Japan, and the Owens Valley Solar Array in California. Observations during the present solar maximum are a particular focus of this program. Properly interpreted radio data permit determination of many physical parameters, such as coronal magnetic field strengths and the magnetic configurations above active regions, that cannot be obtained by any other technique. Knowledge of these parameters is vital to any models of solar flares and active regions.