en:praktikum:sonnenspektroskopie

Differences

This shows you the differences between two versions of the page.

Link to this comparison view

Both sides previous revision Previous revision
Next revision		 Previous revision
en:praktikum:sonnenspektroskopie [2023/04/25 10:30] – [Report] rhainichen:praktikum:sonnenspektroskopie [2023/07/21 21:28] (current) – [Analysis] rhainich
Line 48: Line 48:
  
 Save the script and execute it by Save the script and execute it by
-  python3 comparespecs.py+  python comparespecs.py
 This will produce a PDF 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 
   okular spectrum.pdf &   okular spectrum.pdf &
Line 71: Line 71:
 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). 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).
  
-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]]. Classify the sunspot following the Waldmeier (Zurich) scheme. +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. 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? 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}}.
  
 /* /*
  • en/praktikum/sonnenspektroskopie.1682418603.txt.gz
  • Last modified: 2023/04/25 10:30
  • by rhainich