Hostname: page-component-586b7cd67f-r5fsc Total loading time: 0 Render date: 2024-11-23T14:31:23.136Z Has data issue: false hasContentIssue false
  • English
  • Français

An Extra-Solar Planet in a Double Stellar System: The Modelling of Insufficient Orbital Elements

Published online by Cambridge University Press:  23 April 2012

Eva Plávalová ,
Nina A. Solovaya  and
Eduard M. Pittich
Eva Plávalová
Affiliation:
Dept. of Astronomy, Earth's Physics, and Meteorology, Comenius University, Bratislava, Slovak Republic, email: [email protected]
Nina A. Solovaya
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, Bratislava, Slovak Republic email: [email protected], [email protected] Sternberg Astronomical Institute, Moscow State University, Moscow, Russia email: [email protected]
Eduard M. Pittich
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, Bratislava, Slovak Republic email: [email protected], [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.

The modelling of the insufficient orbital elements of extra-solar planets (EPs) revolving around one component in a binary star system is investigated in the present paper. This problem is considered in the frame of the three-body problem using the analytical theory of Orlov & Solovaya (1998). In the general case, the motion is defined by the masses of the components and by the six pairs of the initial values of the Keplerian elements. For EPs, it is not possible to obtain the complete set of elements for the orbit, in particular, the ascending node and the angle of the inclination. So, it is possible the two different variants of orbital evolution of EPs depend on the initial conditions. In one case, the orbit is unstable. Using the stability conditions of Solovaya & Pittich (2004), which are presented by the angle of the mutual inclination of the orbits between the EP and distant star, we varied unknown angular elements and defined the regions with possible values of the elements for which the motion of EP stays stable. We applied these calculations to the particular specific EPs: HD19994b, HD196885Ab and HD222404b.

Keywords

three body problemorbital stability of extra-solar planetsHD19994bHD196885Ab and HD222404b
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 127 - 128
Copyright
Copyright © International Astronomical Union 2012

References

Hartkopf, W. I. & Mason, B. D. 2001, Sixth Catalog of Orbits of Visual Binary StarsGoogle Scholar
Chauvin, G., Beust, H., Lagrange, A.-M., & Eggenberger, A. 2011, A&A, 528, A8Google Scholar
Orlov, A.A. & Solovaya, N.A. 1998, in The Few Body Problem, ed. Valtonen, M.J., (Kluwer Acad. Publish., Dordrecht), 243Google Scholar
Schneider, J. 2011, Extra-solar Planets Catalogue, http://exoplanet.euGoogle Scholar
Solovaya, N.A. & Pittich, E.M. 2004, Contrib. Astron. Obs. Skalnaté Pleso, 34, 105Google Scholar
Torres, G. 2008, arXiv:astro-ph/0609638v1Google Scholar