Solar Spectropolarimetry and Diagnostic Techniques

Monday, September 24, 2018 to Friday, October 5, 2018

The registration is now closed and participants have been selected.

The polarized spectrum of the Sun encodes a wealth of information on the thermodynamic and magnetic properties of its atmosphere, which ultimately drive all phenomena of Space Weather affecting the Earth and near-Earth environment. In order to unveil this valuable information, scientists must perform critically sensitive spectro-polarimetric observations of the Sun, and then carefully reduce, analyze, and interpret the observed data. However, all the aspects involved in this effort (theory, modeling, instrumentation, data analysis) constitute a highly specialized craft, which is notoriously difficult to master.

This two-week school aims at presenting a comprehensive overview of the field of solar spectropolarimetry, and the the various tools and methods necessary for decoding the polarization of the solar spectrum.

This school will take place 24 September - 5 October of 2018 in Estes Park, Colorado. The organization will (at least partially) support travel and accommodation costs for the students. This is possible thanks to our sponsors: the High Altitude Observatory of NCAR, the Advanced Study Program of NCAR, and the National Solar Observatory.

Intended audience

This school is designed for people who want to delve into the field of spectropolarimetry and learn to carry out spectral line inversions of photospheric and chromospheric (and some coronal) spectra.

  • If you are a solar physicist that doesn't know anything about spectropolarimetry but would like to learn what it's all about, this school is for you.
  • If you use an inversion code as a black box for your data analysis, but you'd like to learn the underlying theory, physical processes and how inversions actually work, then this school is for you.
  • If you have an understanding of the theory of polarized radiative transfer but you'd like to learn about the instrumentation used to acquire the observations and the limitations that arise from the quirks of the data, this school is for you.
  • If you have used a Milne-Eddington inversion code in the past, but you'd like to be able to extract more information from your data (thermodynamical properties and atmospheric stratification), then this school is for you.

Structure of the school

The first week of the school intends to equip the participants with the basic knowledge of how polarization is produced in the Sun and measured with our instruments. We will delve into the theory of radiative transfer to understand how the polarized light is actually generated and modified as it propagates through the Sun’s atmosphere, and at the same time we will describe the typical optical devices and instrumentation techniques that enable the measurement of the Sun’s polarized spectrum. You can find more detailed information about the school syllabus here.

In the second week, the participants will learn how the theoretical and modeling concepts acquired during the first week are used in practice to extract information about the physical conditions of the Sun’s atmosphere. We will present three different spectral-line inversion codes, with guided tutorials involving hands-on activities, with the goal of developing a working understanding of these software packages and their use for the analysis of spectropolarimetric observations. You can find descriptions of the three inversion codes here.

The school will rely on lectures as well as instrumentation and computer lab tutorials taught by leading world experts. The experience will not only offer the participants the opportunity to dive into the field of spectropolarimetry, but will also enable them to develop a network of connections with fellow students, experts, and mentors alike.

For further information please email Rebecca Centeno (rce at ucar dot edu).