English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We study the orbital stability of a non-zero mass, close-in circular orbitplanet around an eccentric orbit binary for various initial values of thebinary eccentricity, binary mass fraction, planet mass, planet semi--majoraxis, and planet inclination by means of numerical simulations that cover $5\times 10^4$ binary orbits. For small binary eccentricity, the stable orbitsthat extend closest to the binary (most stable orbits) are nearly retrogradeand circulating. For high binary eccentricity, the most stable orbits arehighly inclined and librate near the so-called generalised polar orbit which isa stationary orbit that is fixed in the frame of the binary orbit. For moreextreme mass ratio binaries, there is a greater variation in the size of thestability region (defined by initial orbital radius and inclination) withplanet mass and initial inclination, especially for low binary eccentricity.For low binary eccentricity, inclined planet orbits may be unstable even atlarge orbital radii (separation $> 5 \,a_{\rm b}$). The escape time for anunstable planet is generally shorter around an equal mass binary compared withan unequal mass binary. Our results have implications for circumbinary planetformation and evolution and will be helpful for understanding futurecircumbinary planet observations.

Polar planets around highly eccentric binaries are the most stable