en:praktikum:sonnenspektroskopie

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en:praktikum:sonnenspektroskopie [2016/07/01 00:36] – rhainichen:praktikum:sonnenspektroskopie [2023/07/21 21:28] (current) – [Analysis] rhainich
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 Estimate the magnetic field strength in a sunspot, using the Zeeman splitting of spectral lines.  Estimate the magnetic field strength in a sunspot, using the Zeeman splitting of spectral lines. 
  
 +===== Observation =====
 +The observation will be performed with the solar telescope in the "Einsteinturm". 
 ===== Data reduction ===== ===== Data reduction =====
  
-Login at the [[en:praktikum:zugang | Laboratory Course computer]]. Copy the observational data (TIFF files) from the directory ''~/daten/<date>''  to your own directory (see [[en:praktikum:namenskonvention|name conventions]]). Use the command ''ls'' to view the directory's content. After the copying there should be at least two TIFF files, possibly with names that represent the meaning of the image.+++++ Data reduction for data taken before 2016: | 
 + 
 +Login at the [[en:praktikum:zugang | Laboratory Course computer]]. Copy the observational data (TIFF files) from the directory ''~/data/<date>''  to your own directory (see [[en:praktikum:namenskonvention|name conventions]]). Use the command ''ls'' to view the directory's content. After the copying there should be at least two TIFF files, possibly with names that represent the meaning of the image.
  
 The TIFF images can be viewed in //ImageMagick// with the console command The TIFF images can be viewed in //ImageMagick// with the console command
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 (The default contrast settings are generally unfavorable, as the image appears extremely dark.) (The default contrast settings are generally unfavorable, as the image appears extremely dark.)
  
- We use [[en:praktikum:gdl|GDL]] for the data reduction. The program need to do the following steps:+ We use //[[en:praktikum:gdl|GDL]]// for the data reduction. The program need to do the following steps:
   * Convert TIFF to FITS    * Convert TIFF to FITS 
   * Read-in the FITS file   * Read-in the FITS file
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 Luckily, the required program (''konvert.pro'') is already prepared and can be found in the scripts directory. Copy it to your own directory. At the end of this program a few lines need to be adjusted. Use a text editor, i.e. Luckily, the required program (''konvert.pro'') is already prepared and can be found in the scripts directory. Copy it to your own directory. At the end of this program a few lines need to be adjusted. Use a text editor, i.e.
   kate konvert.pro &   kate konvert.pro &
-to open the script and change the parameters that describe the input files (filenames, dimensions). To compile the program, start GDL+to open the script and change the parameters that describe the input files (filenames, dimensions). To compile the program, start //GDL//
   gdl   gdl
 then compile the program via then compile the program via
   gdl> .compile konvert.pro   gdl> .compile konvert.pro
-The program itself is started in GDL by calling the program name, which in this case should be+The program itself is started in //GDL// by calling the program name, which in this case should be
   gdl> konvert   gdl> konvert
  
-The program converts and rotates the images, then saves the FITS files. They can be viewed (outside of GDL) with +The program converts and rotates the images, then saves the FITS files. They can be viewed (outside of //GDL//) with 
   ds9 filename.fits &   ds9 filename.fits &
 The image should be clearer and rotated in comparison to the TIFF file.  The image should be clearer and rotated in comparison to the TIFF file. 
  
 +++++
  
 ===== Analysis ===== ===== Analysis =====
 +
 +{{section>deng:praktikum:a12:python#English&noheader}}
  
 The analysis can be performed with the Python script //comparespecs.py// that is already known from S1. The input (filename, lines) need to be adjusted accordingly. Use an editor of your choice. Note, that both spectra are in one file now. Mind that pixel errors can best be avoided by averaging over a number of lines of the image, but choose the regions with the maximal splitting. The analysis can be performed with the Python script //comparespecs.py// that is already known from S1. The input (filename, lines) need to be adjusted accordingly. Use an editor of your choice. Note, that both spectra are in one file now. Mind that pixel errors can best be avoided by averaging over a number of lines of the image, but choose the regions with the maximal splitting.
  
 Save the script and execute it by Save the script and execute it by
-  ./comparespecs.py +  python comparespecs.py 
-This will produce a PostScript file with the overlaid spectra which can be viewed with  +This will produce a PDF file with the overlaid spectra which can be viewed with  
-  gv speccmp.ps &+  okular spectrum.pdf &
 To avoid overwriting the output of S1 it is possible to change the filename of the output. Determine the shift of the Zeeman components $\Delta \lambda$. The wavelength calibration is done using telluric oxygen lines (see Table below). The magnetic field strength can then be calculated: To avoid overwriting the output of S1 it is possible to change the filename of the output. Determine the shift of the Zeeman components $\Delta \lambda$. The wavelength calibration is done using telluric oxygen lines (see Table below). The magnetic field strength can then be calculated:
  
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 | Fe  |  630.151  | $g = \frac{5}{3}$ | | Fe  |  630.151  | $g = \frac{5}{3}$ |
 | Fe  |  630.250  | $g = \frac{5}{2}$ | | Fe  |  630.250  | $g = \frac{5}{2}$ |
 +| O<sub>2</sub>  |  629.846  |   |
 +| O<sub>2</sub>  |  629.923  |   |
 | O<sub>2</sub>  |  630.200  |   | | O<sub>2</sub>  |  630.200  |   |
 | O<sub>2</sub>  |  630.276  |   | | O<sub>2</sub>  |  630.276  |   |
  
-===== Protocol =====+===== Report =====
  
-//Note, a joined protocol shall be created for S1 and S2.//+A combined report for [[https://polaris.astro.physik.uni-potsdam.de/wiki/doku.php?id=en:praktikum:sonnenrotation#report|S1]] and S2 with the usual content is to be handed in. See a general overview about the required structure and content [[https://polaris.astro.physik.uni-potsdam.de/wiki/doku.php?id=en:praktikum:protocol|here]].
  
-The protocol is expected to contain the basic theory of the Zeeman effect. The above formula is to be derived. Discuss the importance of the Zeeman effect for this laboratory course. Search for an image of the investigated sunspots in the [[http://sohowww.nascom.nasa.gov/|SOHO-Archive]]. Classify the sunspot following the Waldmeier (Zurich) scheme.  +For this experiment, the theoretical overview in the report should give a short introduction to the //Einsteinturm// and its instrumentation. Describe how the rotation of the sun is calculated from an observable line shift and the physical background behind it. Mention further geometric corrections that need to be accounted for. Then describe the basics for the Zeeman effect and how we use it in this experiment. This includes a derivation of the formula above. Discuss the importance of the Zeeman splitting for this laboratory course (e.g. which polarization components are visible and which are measured in our observation). 
-/*Reference? 1989JALPO..33...10H or 1961says.book.....W */+ 
 +In the methods section, describe the observations and the data extraction, highlight points that deviate from general description in here, and list all the parameters you set for the extraction. Search for an image of the investigated sunspots in the [[http://sohowww.nascom.nasa.gov/|SOHO-Archive]] or using [[https://suntoday.lmsal.com/suntoday/|Sun in time]]. Classify the sunspot following the Waldmeier (Zurich) scheme.  
 + 
 +The results and analysis part presents the extracted solar spectra. It also includes the measurement of the radial velocity shift and the line splitting.  Do not forget to list the individual lines that you use with their respective rest frame wavelength, line shift, etc. Calculate the solar rotation and the strength of the magnetic field. 
 + 
 +Finally, discuss your findings. Bring your results into a larger context and make a literature comparison to known solar rotation period and typical magnetic field strength in sun spots. This also includes that you identify potential problems with the data, the data reduction, or the analysis and possible solutions for them. Are their inconsistencies? Do your resulting period and field strength match your expectations? If not, what are potential reason for that? 
 + 
 +Further tips on how to handle writing the reports can be found in {{en:labcourse:talks:s1s2_presentation_fmattig.pdf|this presentation}}. 
 + 
 +/* 
 +**OLD BELOW** 
 + 
 +//Note, a joined report shall be created for S1 and S2.// 
 + 
 +The report is expected to contain the basic theory of the Zeeman effect. The above formula is to be derived. Discuss the importance of the Zeeman splitting for this laboratory course (e.g. which polarization components are visible and which are measured in our observation). Search for an image of the investigated sunspots in the [[http://sohowww.nascom.nasa.gov/|SOHO-Archive]]. Classify the sunspot following the Waldmeier (Zurich) scheme.  
 +Reference? 1989JALPO..33...10H or 1961says.book.....W
 Calculate the magnetic field strength in the sunspot and discuss its plausibility in regard to comparison values. Calculate the magnetic field strength in the sunspot and discuss its plausibility in regard to comparison values.
 +*/
 +
 +=== Recommended Literature ===
 +
 +Zeeman effect: //Joachim Stöhr - Magnetism: From Fundamentals to Nanoscale Dynamics// (available at Golm Libaray, IKMZ)
  
 [[en:praktikum:index|Overview: Laboratory courses]] [[en:praktikum:index|Overview: Laboratory courses]]
  
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