Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-25T16:42:53.662Z Has data issue: false hasContentIssue false
  • English
  • Français

Using exoplanet systems with highly elliptical orbits to search for star-planet interactions

Published online by Cambridge University Press:  06 January 2014

John R. Hodgson II ,
Damian J. Christian ,
Dennis Bodewits  and
Suzanne Hawley
John R. Hodgson II
Affiliation:
California State University, Northridge, Physics Department, 18111 Nordhoff St, Northridge, California 91330-8268, USA email: [email protected] & [email protected]
Damian J. Christian
Affiliation:
California State University, Northridge, Physics Department, 18111 Nordhoff St, Northridge, California 91330-8268, USA email: [email protected] & [email protected]
Dennis Bodewits
Affiliation:
Department of Astronomy, University of Maryland, College Park, MD 20742, USA email: [email protected]
Suzanne Hawley
Affiliation:
Astronomy Department University of Washington, Box 351580, Seattle, WA 98195, USA email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We are investigating if the orbital geometry of exoplanets affects the activity of their host star by studying a sample of planetary systems known to contain massive planets on short period, highly elliptical orbits. While recent studies in the optical, UV, and X-Ray have shown enhanced chromospheric activity for stars hosting exoplanets with orbital semi-major axes less than 0.1 AU (Krejcova 2012, Shkolnik 2013, Kashyap 2008, Poppenhaeger 2010), it is not yet clear whether this activity is driven by magnetic or tidal interactions. We are probing the dependence of star-planet interactions (SPI) on the orbital geometry of the planetary systems by analyzing chromospheric lines (such as Ca II H & K) for variability phased with the exoplanet's orbit. We have obtained high resolution spectra of several systems with the McDonald 2.1-m Sandiford echelle spectrograph, ARCES on the APO 3.5-m, and for HIRES on Keck I from the Keck Observatory Archive. We describe our methodology and review how our results will use orbital geometry to deduce how planets may affect the activity of their host stars.

Keywords

stars: activitystars: magnetic fieldsplanetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S299: Exploring the Formation and Evolution of Planetary Systems , June 2013 , pp. 291 - 292
Copyright
Copyright © International Astronomical Union 2013 

References

Gurdemir, L., Redfield, S., & Cuntz, M. 2012, PASA, 29, 141CrossRefGoogle Scholar
Kashyap, V. L., Drake, J. J., & Saar, S. H. 2008, ApJ, 687, 1339CrossRefGoogle Scholar
Krejcova, T. 2012, A&A, 540, 82Google Scholar
Poppenhaeger, K., Robrade, J., & Schmitt, J. H. 2010, A&A, 515, A98Google Scholar
Shkolnik, E., Bohlender, D. A., Walker, G. A. H., et al. 2008, ApJ, 676, 628Google Scholar
Shkolnik, E. 2013, ApJ, 766, 9SCrossRefGoogle Scholar
Valenti, J. A., Piskunov, N. 1996, A&AS, 118, 595Google Scholar