Abstract
More than half of all main sequence stars, and an even larger fraction of pre-main sequence stars, reside in binary or multiple systems (Duquennoy and Mayor 1991; Mathieu et al. 2000). The presence of planet-forming material has been indirectly observed around one or both components of some young binaries, and (Mathieu et al. 2000) numerical simulations of the formation of binary stars suggest that disks form within these systems, as well (Bodenheimer et al. 2000). Terrestrial planets and the cores of giant planets are thought to form by an accretion process within a disk of dust and gas (Safronov 1969; Lissauer 1993), and therefore may be common in binary star systems. In this chapter, we present the results from numerical simulations of the final stages of terrestrial planet formation around one or both stars of a binary.
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Acknowledgements
Primary support for this research was provided by the NASA Astrobiology Institute under the NASA Ames Investigation “Linking our Origins to our Future”. We are grateful for the contributions from our collaborators Fred C. Adams, John E. Chambers, and Martin J. Duncan, and we thank Michael J. Way for providing additional CPUs at NASA ARC. E.V.Q. received support in various stages of this research from NASA GSRP, NAS/NRC and NASA NPP fellowships, and the University of Michigan through the Michigan Center for Theoretical Physics (MCTP).
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Quintana, E.V., Lissauer, J.J. (2010). Terrestrial Planet Formation in Binary Star Systems. In: Haghighipour, N. (eds) Planets in Binary Star Systems. Astrophysics and Space Science Library, vol 366. Springer, Dordrecht. https://doi.org/10.1007/978-90-481-8687-7_10
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DOI: https://doi.org/10.1007/978-90-481-8687-7_10
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