Planet formation in binary stars: the case ofγCephei

2008/05/09 by W. Kley, Wilhelm Kley, Richard Nelson +1
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Binary number #Binary star #Binary system #Eccentricity (behavior) #Exoplanet #Gravitation #Perturbation (astronomy) #Planet #Planetary system #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.1051/0004-6361:20079324

12 pages, 17 figures, accepted by Astronomy & Astrophysics

arxiv created 2008/05/09 · openalex publication_date 2008/05/15 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

Context. Over 30 planetary systems have been discovered to reside in binary stars. As some of the binary separations are smaller than 20 astronomical units (AU) the gravitational perturbation of the secondary star has a very strong influence on the planet formation process, as it truncates the protoplanetary disc, possibly shortens its lifetime, and stirs up the embedded planetesimals. Due to its small semi-major axis (18.5 AU) and relatively large eccentricity the binary star γ Cephei represents a particularly challenging example worthy of study in greater detail.

Citations

• A Planetary Companion to γ Cephei A
• Four new wide binaries among exoplanet host stars
• Gas Giant Protoplanets Formed by Disk Instability in Binary Star Systems
• Direct detection of exoplanet host star companionγCep B and revised masses for both stars and the sub-stellar object
• No evidence of a hot Jupiter around HD 188753 A
• Dynamical Stability and Habitability of the γ Cephei Binary‐Planetary System
• Statistical properties of exoplanets
• Properties of planets in binary systems