Protostars and Planets VI, Heidelberg, July 15-20, 2013
Circumstellar Habitable Zones in Tight Binary Star Systems
Pilat-Lohinger, Elke (Institute of Astrophysics, University of Vienna, Austria)
Funk, Barbara (Institute of Astrophysics, University of Vienna, Austria)
Eggl, Siegfried (IMCCE, Paris, France)
The fact that up to 70% of all stellar systems in our Galaxy may not be single-stellar but multi-stellar systems and the growing number of detected planets in binary star systems require methods for a quick assessment of possible habitability of a terrestrial planet in binary star systems.
Concerning planetary motion in a binary star system we distinguish between S-type or circumstellar motion -- where the planet orbits one of the two stars -- and P-type or circumbinary motion -- where the planet orbits both stars. This study is restricted to S-type motion.
First we applied the method of Eggl et al. (2012) and calculated the habitable zone(HZ) of a K-M binary star, where the combined gravitational and radiative influence plays an important role.
Then we added a giant planet and analysed the perturbations of the giant planet and the secondary star, where mean motion resonances and secular resonances can be observed. Finally, we studied the tight binary star system HD41004 AB (a K-M binary) which habors a giant planet. We determined the conditions of this system to host a habitable planet.
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