Long-term stability of planets in and around binary stars
arXiv:2108.07815 · doi:10.1093/mnras/stab2324
Abstract
Planets are observed to orbit the component star(s) of stellar binary systems on so-called circumprimary or circumsecondary orbits, as well as around the entire binary system on so-called circumbinary orbits. Depending on the orbital parameters of the binary system a planet will be dynamically stable if it orbits within some critical separation of the semimajor axis in the circumprimary case, or beyond some critical separation for the circumbinary case. We present N-body simulations of star-forming regions that contain populations of primordial binaries to determine the fraction of binary systems that can host stable planets at various semimajor axes, and how this fraction of stable systems evolves over time. Dynamical encounters in star-forming regions can alter the orbits of some binary systems, which can induce long-term dynamical instabilities in the planetary system and can even change the size of the habitable zone(s) of the component stars. However, the overall fraction of binaries that can host stable planetary systems is not greatly affected by either the assumed binary population, or the density of the star-forming region. Instead, the critical factor in determining how many stable planetary systems exist in the Galaxy is the stellar binary fraction - the more stars that are born as singles in stellar nurseries, the higher the fraction of stable planetary systems.
13 pages, 7 figures, 2 short appendices, accepted for publication in MNRAS. A video abstract created by Helena Gibbon is available here: https://youtu.be/76kANnTK9-s
References in corpus (18)
- A Spitzer Survey of Young Stellar Clusters within One Kiloparsec of the Sun: Cluster Core Extraction and Basic Structural Analysis
- Comparative statistics and origin of triple and quadruple stars
- The M-dwarfs in Multiples (MinMs) survey - I. Stellar multiplicity among low-mass stars within 15 pc
- IN-SYNC II: Virial Stars from Sub-Virial Cores -- The Velocity Dispersion of Embedded Pre-Main-Sequence Stars in NGC 1333
- Dense Stellar Populations: Initial Conditions
- Planetary Systems in Binaries. I. Dynamical Classification
- The Evolution of the Multiplicity of Embedded Protostars II: Binary Separation Distribution & Analysis
- A case of simultaneous star and planet formation
- Cluster dynamics largely shapes protoplanetary disc sizes
- Dynamics versus structure: breaking the density degeneracy in star formation
- The instability of planetary systems in binaries: how the Kozai mechanism leads to strong planet-planet interactions
- Binaries in the field: fossils of the star formation process?
- Orbital Stability of Circumstellar Planets in Binary Systems
- Rapid destruction of protoplanetary discs due to externalphotoevaporation in star-forming regions
- Implementing Primordial Binaries in Simulations of Star Cluster Formation with a Hybrid MHD and Direct N-Body Method
- Revisiting the universality of (multiple) star formation in present-day star formation regions
- On the enlargement of habitable zones around binary stars in hostile environments
- Enlarging habitable zones around binary stars in hostile environments