[English]

Prosiectau Ffiseg ar gyfer myfyrwyr bl.3 a bl.4


Disgrifiad prosiect

Mapping the solar temperature minimum region

(supervisor: David Kuridze)

Nature of project: data analysis, data analysis

Available to students on full-time physics degree schemes or joint students.

Project description and methodology

The Sun has a complicated temperature structure. The heat producing core of the Sun has a very high temperature of more that 15 million Kelvin. As we move away from the core the temperature drops to about 5,800 Kelvins at the photosphere, the effective (visible) surface of the Sun. Then it drops to a minimum about 4,000 K at approximately 500 kilometres above the photosphere. The temperature then rises again to more than several million degrees in the corona which is the outer layer of the Sun's atmosphere.

The aim of this project is to investigate the formation height and width of the temperature minimum region above the surface of the Sun. The student will use a high-resolution spectroscopic data observed off-limb with the Swedish 1-m Solar Telescope. The data will be used to find intensity dip produced by the temperature minimum region in the hydrogen beta line. This dip maps the temperature minimum between photosphere and chromosphere. Formation height above the surface and width of the temperature minumum will be directly measured from this dip.

A successful project will develop beyond the above in one/some of the following directions:
The main way to develop this project further is to compare the observations with synthetic Hbeta off limb data computed with the numerical code.

When considering where to take your project, please bear in mind the time available. It is preferable to do fewer things well than to try many and not get conclusive results on any of them. However, sometimes it is useful to have a couple of strands of investigation in parallel to work on in case delays occur.

This project is only available as a Y3 project.

Please speak to David Kuridze (dak21) if you consider doing this project.

Initial literature for students:

  1. The Sun as a Guide to Stellar Physics, Editors: Oddbjørn Engvold Jean-Claude Vial Andrew Skumanich, Chapter 3, page 59-72
  2. An Introduction to Modern Astrophysics, Bradley W Carroll, Dale A Ostlie (authors), Chapter: The Sun, page 321 - 341
  3. Leenaarts, J.; Carlsson, M.; Rouppe van der Voort, L., The Formation of the Hα Line in the Solar Chromosphere, Astrophysical Journal, DOI: 10.1088/0004-637X/749/2/136, 2006

Novelty, degree of difficulty and amount of assistance required

Fully processed imaging spectroscopy data and assistance how to analyse it will be provided. IDL/Python training will be provided by the supervisor.

Project milestones and deliverables (including timescale)

milestoneto be completed by
The basic structure of the of the solar atmosphere (overview)end of October
Learning how to open/load the data in IDL and develop the codeChristmas
Mapping the temperature minimum using the IDL codeend of February
Determine the formation height and width of the temperature minimum region above the surfaceEaster