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Dynamics and Habitability in Binary Star Systems

Published online by Cambridge University Press:  05 January 2015

Siegfried Eggl ,
Nikolaos Georgakarakos  and
Elke Pilat-Lohinger
Siegfried Eggl
Affiliation:
IMCCE, Observatoire de Paris, 77 Avenue Denfert-Rochereau, F-75014, Paris, France email: [email protected]
Nikolaos Georgakarakos
Affiliation:
Higher Technological Educational Institute of Central Macedonia, Terma Magnesias, Serres 62124, Greece email: [email protected]
Elke Pilat-Lohinger
Affiliation:
University of Graz, Institute of Physics, IGAM, Universitätsplatz 5, 8010 Graz, Austria email: [email protected]
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Abstract

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Determining planetary habitability is a complex matter, as the interplay between a planet's physical and atmospheric properties with stellar insolation has to be studied in a self consistent manner. Standardized atmospheric models for Earth-like planets exist and are commonly accepted as a reference for estimates of Habitable Zones. In order to define Habitable Zone boundaries, circular orbital configurations around main sequence stars are generally assumed. In gravitationally interacting multibody systems, such as double stars, however, planetary orbits are forcibly becoming non circular with time. Especially in binary star systems even relatively small changes in a planet's orbit can have a large impact on habitability. Hence, we argue that a minimum model for calculating Habitable Zones in binary star systems has to include dynamical interactions.

Keywords

stars: binariesstars: planetary systemshabitabilitycelestial mechanics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S310: Complex Planetary Systems , July 2014 , pp. 53 - 57
Copyright
Copyright © International Astronomical Union 2014 

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