The 19th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun
Published August 1, 2016 | Version v1
Presentation Open

Probing Stellar Dynamics with Space Photometry

Authors/Creators

  • 1. Laboratoire AIM, CEA/DRF-CNRS, Université Paris 7 Diderot, IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette, France
  • 2. Université de Toulouse, UPS-OMP, IRAP, 31400 Toulouse, France
  • 3. Laboratoire Lagrange, UMR7293, Université de la Côte d’Azur, CNRS, Observatoire de la Côte d’Azur, Nice, France
  • 4. High Altitude Observatory, National Center for Atmospheric Research, PO Box 3000, Boulder, CO 80307-3000, USA
  • 5. Instituto de Astrofisica de Canarias, 38205, La Laguna, Tenerife, Spain
  • 6. Space Science Institute, 4750 Walnut street Suite#205, Boulder, CO 80301, USA
  • 7. Universidade Federal do Rio Grande do Norte, UFRN, Dep. de Física, DFTE, CP1641, 59072-970, Natal, RN, Brazil

Contributors

  • 1. Uppsala University, University of North Georgia
  • 2. Max Planck Institute for Solar System Research
  • 3. University of Geneva
  • 4. Aarhus University
  • 5. National Solar Observatory
  • 6. University of Copenhagen
  • 7. Konkoly Observatory
  • 8. Trinity College Dublin
  • 9. Instituto de Astrofísica de Canarias

Description

The surface magnetic field has substantial influence on various stellar properties that can be probed through various techniques. With the advent of new space-borne facilities such as CoRoT and Kepler, uninterrupted long high-precision photometry is available for hundred of thousand of stars. This number will substantially grow through the forthcoming TESS and PLATO missions. The unique Kepler observations –covering up to 4 years with a 30-min cadence– allows studying stellar variability with different origins such as pulsations, convection, surface rotation, or magnetism at several time scales from hours to years. We study the photospheric magnetic activity of solar-like stars by means of the variability induced in the observed signal by starspots crossing the visible disk. We constructed a solar photometric magnetic activity proxy, Sph from SPM/VIRGO/SoHO, as if the Sun was a distant star and we compare it with several solar well-known magnetic proxies. The results validate this approach. Thus, we compute the Sph proxy for a set of CoRoT and Kepler solar-like stars for which pulsations were already detected. After characterizing the rotation and the magnetic properties of 300 solar-like stars, we use their seismic properties to characterize 18 solar analogs for which we study their magnetism. This allows us to put the Sun into context of its siblings.

Notes

Contributed talk at the Splinter Session on "Variability of Solar/Stellar Magnetic Activity" (http://coolstars19.com/splinters/stellar-var/index.html) at the "Cool Stars 19" Workshop

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