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A magnetic cycle of τ Bootis? The coronal and chromospheric view

  1. K. Poppenhaeger1,*,
  2. H.M. Günther2,
  3. J.H.M.M. Schmitt1

Article first published online: 12 JAN 2012

DOI: 10.1002/asna.201111614

Issue

Astronomische Nachrichten

Astronomische Nachrichten

Volume 333, Issue 1, pages 26–29, January 2012

Additional Information

How to Cite

Poppenhaeger, K., Günther, H.M. and Schmitt, J.H.M.M. (2012), A magnetic cycle of τ Bootis? The coronal and chromospheric view. Astron. Nachr., 333: 26–29. doi: 10.1002/asna.201111614

Author Information

  1. 1

    Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany

  2. 2

    Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

*Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany

Publication History

  1. Issue published online: 12 JAN 2012
  2. Article first published online: 12 JAN 2012
  3. Manuscript Accepted: 6 OCT 2011
  4. Manuscript Received: 19 SEP 2011

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Keywords:

  • stars: activity;
  • stars: coronae;
  • stars: chromospheres;
  • stars: individual (HD 120136);
  • X-rays: stars

Abstract

τ Bootis is a late F-type main sequence star orbited by a Hot Jupiter. During the last years spectropolarimetric observations led to the hypothesis that this star may host a global magnetic field that switches its polarity once per year, indicating a very short activity cycle of only one year duration. In our ongoing observational campaign, we have collected several X-ray observations with XMM-Newton and optical spectra with TRES/FLWO in Arizona to characterize τ Boo's corona and chromosphere over the course of the supposed one-year cycle. Contrary to the spectropolarimetric reconstructions, our observations do not show indications for a short activity cycle (© 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

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