EWASS Special Session 4 (2017): Star-planet interactions
Published October 13, 2017 | Version v2
Conference paper Open

Tidal dissipation in rotating low mass stars: implications for the orbital evolution of close in planets

Authors/Creators

  • 1. Department of Astronomy, University of Geneva, Chemin des Maillettes 51, 1290 Versoix, Switzerland
  • 2. Laboratoire AIM Paris-Saclay, CEA/DRF - CNRS - Univ. Paris Diderot - IRFU/SAp, Centre de Saclay, 91191 Gif-sur-Yvette Cedex, France
  • 3. Physikalisches Institut & Center for Space and Habitability, Universitaet Bern, 3012 Bern, Switzerland

Contributors

  • 1. Laboratoire AIM Paris-Saclay, CEA/DRF - CNRS - Université Paris Diderot, IRFU/SAp Centre de Saclay, 91191, Gif-sur-Yvette
  • 2. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

Description

Close-in planets represent a large fraction of the population of conVrmed exoplanets. To understand the dynamical evolution
of these planets, star-planet interactions must be taken into account. In particular, the dependence of the tidal interactions
on the structural parameters of the star, its rotation, and its metallicity should be treated in the models. We quantify how
the tidal dissipation in the convective envelope of rotating low-mass stars evolves in time. We also investigate the possible
consequences of this evolution on planetary orbital evolution. In Gallet et al. (2017) and Bolmont et al. (2017) we generalized
the work of Bolmont & Mathis (2016) by following the orbital evolution of close-in planets using the new tidal dissipation
predictions for advanced phases of stellar evolution and non-solar metallicity.
We Vnd that during the pre-main sequence the evolution of tidal dissipation is controlled by the evolution of the internal
structure of the star through the stellar contraction. On the main-sequence tidal dissipation is strongly driven by the evolution
of the surface rotation that is impacted by magnetized stellar winds braking. Finally, during the more evolved phases, the tidal
dissipation sharply decreases as radiative core retreats in mass and radius towards the red-giant branch.
Using an orbital evolution model, we also show that changing the metallicity leads to diUerent orbital evolutions (e.g., planets
migrate farther out from an initially fast rotating metal rich star). By using this model, we qualitatively reproduced the
observational trends of the population of hot Jupiters with the metallicity of their host stars. However, more work still remain
to be do so as to be able to quantitatively Vt our results to the observations.

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References

  • Adibekyan, V. Z., Figueira, P., Santos, N. C., Mortier, A., Mordasini, C., et al. 2013, A&A, 560, A51.
  • Alibert, Y., Carron, F., Fortier, A., PfyUer, S., Benz, W., et al. 2013, A&A, 558, A109.
  • Amard, L., Palacios, A., Charbonnel, C., Gallet, F., & Bouvier, J. 2016, A&A, 587, A105.
  • Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481.
  • Barker, A. J. & Ogilvie, G. I. 2010, MNRAS, 404, 1849.
  • Beaugé, C. & Nesvorný, D. 2013, ApJ, 763, 12.
  • Bolmont, E., Gallet, F., Mathis, S., Charbonnel, C., Amard, L., et al. 2017, A&A, 604, A113.
  • Bolmont, E. & Mathis, S. 2016, Celestial Mechanics and Dynamical Astronomy, 126, 275.
  • Bolmont, E., Raymond, S. N., Leconte, J., & Matt, S. P. 2012, A&A, 544, A124.
  • Charbonneau, D., Brown, T. M., Latham, D. W., & Mayor, M. 2000, ApJL, 529, L45.
  • Choi, J., Dotter, A., Conroy, C., Cantiello, M., Paxton, B., et al. 2016, ApJ, 823, 102.
  • Fabrycky, D. C., Lissauer, J. J., Ragozzine, D., Rowe, J. F., SteUen, J. H., et al. 2014, ApJ, 790, 146.
  • Gallet, F., Bolmont, E., Mathis, S., Charbonnel, C., & Amard, L. 2017, A&A, 604, A112.
  • Gallet, F. & Bouvier, J. 2015, A&A, 577, A98.
  • Gonzalez, G. 1997, MNRAS, 285, 403.
  • Ida, S. & Lin, D. N. C. 2004, ApJ, 616, 567.
  • Johnson, J. L. & Li, H. 2012, ApJ, 751, 81.
  • Johnstone, C. P., Güdel, M., Brott, I., & Lüftinger, T. 2015, A&A, 577, A28.
  • Lagarde, N., Decressin, T., Charbonnel, C., Eggenberger, P., Ekström, S., et al. 2012, A&A, 543, A108.
  • Lanzafame, A. C. & Spada, F. 2015, A&A, 584, A30.
  • Mathis, S. 2015, A&A, 580, L3.
  • Mayor, M. & Queloz, D. 1995, Nature, 378, 355.
  • Mordasini, C., Alibert, Y., Benz, W., Klahr, H., & Henning, T. 2012, A&A, 541, A97.
  • Mordasini, C., Alibert, Y., Benz, W., & Naef, D. 2009, A&A, 501, 1161.
  • Neves, V., BonVls, X., Santos, N. C., Delfosse, X., Forveille, T., et al. 2013, A&A, 551, A36.
  • Ogilvie, G. I. 2013, MNRAS, 429, 613.
  • Ogilvie, G. I. & Lin, D. N. C. 2007, ApJ, 661, 1180.
  • Pinsonneault, M. H., Kawaler, S. D., & Demarque, P. 1990, ApJS, 74, 501.
  • Reiners, A. & Mohanty, S. 2012, ApJ, 746, 43.
  • Remus, F., Mathis, S., & Zahn, J.-P. 2012, A&A, 544, A132.
  • Santos, N. C., Israelian, G., Mayor, M., Rebolo, R., & Udry, S. 2003, A&A, 398, 363.
  • Strugarek, A. 2016, ApJ, 833, 140.
  • Strugarek, A., Brun, A. S., Matt, S. P., & Réville, V. 2014, ApJ, 795, 86.
  • Terquem, C., Papaloizou, J. C. B., Nelson, R. P., & Lin, D. N. C. 1998, ApJ, 502, 788.
  • Zahn, J. P. 1966, Annales d'Astrophysique, 29, 489.
  • Zahn, J.-P. 1975, A&A, 41, 329.