Collaborative Research: Polarimetric Imaging and Spectroscopy of the Corona from 500-1500nm during Total Solar Eclipses

合作研究：日全食期间 500-1500nm 日冕的偏振成像和光谱学

• 批准号: 0450096
• 负责人: Martina Arndt
• 金额: $ 2.56万
• 依托单位: BRIDGEWATER STATE UNIVERSITY
• 依托单位国家: 美国
• 项目类别: Continuing Grant
• 财政年份: 2005
• 资助国家: 美国
• 起止时间: 2005-02-01 至 2010-01-31
• 项目状态: 已结题
• 来源: https://www.nsf.gov/awardsearch/showAward?AWD_ID=0450096&HistoricalAwards=false
• 关键词: Collaborative; Research; Polarimetric; Imaging; Spectroscopy

The proposed four-year project will take advantage of unique opportunities offered by the total solar eclipses of 29 March 2006 (Libya) and 1 August 2008 (China-Russia) for imaging and spectroscopy of polarized coronal emissions at wavelengths spanning the visible to the near infrared. Polarized emission is a characteristic of some of the strongest coronal emission lines, while polarized fluorescence is a property of nanometer size dust particles. The near infrared polarimetric observations carried out by the PI during the eclipse of 21 June 2001 led to the serendipitous discovery of the signature of nanometer size dust particles in the inner corona. These 2001 observations also pointed to the potential existence of a discrete spectrum resulting from the fluorescence of these dust grains, and their spectrum is likely to be embedded within the spectrum of coronal ionic lines. By observing the next eclipses, the PI plans to infer the direction of the coronal magnetic field at different stages of the solar cycle, uncover the spectrum of nanometer size dust grains in the inner corona, and establish the relationship between interplanetary dust grains and the coronal magnetic field. In addition to the observations from Libya and China-Russia, simultaneous and identical observations will be made with the coronagraph in Hawaii. All the coronal observations will be compared with polarimetric laboratory measurements of fluorescence from silicon nanoparticles, which can be synthesized into stable and reproducible discrete sizes that fluoresce in the blue, green, yellow, and infrared part of the spectrum, under non-resonant UV or resonant excitation of their emission bands. Knowledge of the direction of the coronal field is critical for establishing the fraction of the solar magnetic flux that escapes into interplanetary space carrying the solar wind with it. Embedded in the solar wind, the interplanetary magnetic field shapes the environment of planets and defines the heliosphere. While the field also shapes cometary tails, it is likely to be responsible for the distribution of dust particles in the corona that may come from the sublimation of sun-grazing comets. The proposed program opens a new research direction by exploring the coupled signature of the coronal magnetic field direction and the fluorescence spectrum from nanoparticle dust grains in the inner corona. This effort will complement the laboratory experiments on polarized fluorescence from silicon nanoparticles.

拟议的四年项目将利用2006年3月29日（利比亚）和2008年8月1日（中国俄罗斯）的太阳日食提供的独特机会，用于在可见的近红外线的波长下进行两极分化的冠状发射的成像和光谱。极化发射是一些最强的冠状发射线的特征，而极化荧光是纳米尺寸灰尘颗粒的特性。 PI在2001年6月21日的日食期间进行的近红外偏光观测导致内部电晕中纳米尺寸尘埃颗粒的签名偶然发现。这些2001年的观察结果还表明，由于这些粉尘晶粒的荧光导致了离散光谱的存在，并且它们的光谱很可能嵌入到冠状离子线的光谱中。通过观察下一个日食，PI计划在太阳周期的不同阶段推断冠状磁场的方向，发现内部电晕中纳米尺寸的粉尘粒的光谱，并建立跨层次的粉尘粒与冠状磁场之间的关系。除了从利比亚和中国的观察结果外，还将与夏威夷的Coronagraph进行同时且相同的观察。将将所有冠状观察结果与硅纳米颗粒的荧光测量进行比较，这些硅纳米颗粒可以合成为稳定且可重复的离散大小，这些尺寸在蓝色，绿色，黄色和红外的一部分中，在非共振紫外线或共振抗性或共振的兴奋性兴奋剂中。 了解冠状场的方向对于建立太阳磁通量的比例至关重要，该磁通量逃到了带有太阳风的星际空间中。星际磁场嵌入太阳风中，塑造了行星的环境并定义了地球球。尽管该田也塑造了彗星的尾巴，但它可能是导致电晕中灰尘颗粒的分布，这可能来自阳光般的彗星的升华。提出的程序通过探索冠状磁场方向的耦合特征和内部电晕中纳米颗粒尘埃的荧光光谱来打开新的研究方向。这项工作将补充来自硅纳米颗粒极化荧光的实验室实验。