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Wolf-Rayet Stars

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Manuel Wolff ; Johannes Zabl ; Jürgen Leschhorn
Leonard Storz

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Group 142


Comparison between WR and other, similar early type stars  

  • LBV
    Wolf-Rayet stars are very similar to the LBVs ( L uminous B lue V ariables). Types like S Dor or P Cygni are counted to this group. Both WR and LBV are characterized by their emission lines as a consequence of their stellar winds through which both types lose approximately the same amount of mass.
    One can separate them by their different time scales of variablity. The LBV's need much more time, up to several decades.
    According to the great similarity it seems logical that these stars are assumed as one of the possible predecessors.
  • Of
    These are the hottest, most massive and luminous stars. They can weigh up to 120 solar masses. They are more extreme then WR stars
  • Central Stars of Planetary Nebula
    They have almost equal spectra and similar physical and chemical facts as WC stars. Besides having a wider range of temperature and a higher presence of hydrogen there are no bigger differences. Even the models developed for WC stars fit to this type either.
    But they only pretend being the same. Astronomers have achieved the knowledge that the Central Stars undergo a development that is very different from the Wolf-Rayet stars. As s consequence of their development from red giant stars, they have only a small percentage of the Wolf-Rayet stars' masses.