Oscillations in the habitable zone around α Centauri B


  • Duncan Forgan

    Corresponding author
    1. Scottish Universities Physics Alliance (SUPA), Institute for Astronomy, University of Edinburgh, Blackford Hill, Edinburgh EH9 3HJ
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E-mail: dhf@roe.ac.uk


The α Cen AB system is an attractive one for radial velocity observations to detect potential exoplanets. The high metallicity of both α Cen A and B suggests that they could have possessed circumstellar discs capable of forming planets. As the closest star system to the Sun, with well over a century of accurate astrometric measurements (and α Cen B exhibiting low chromospheric activity), high-precision surveys of α Cen B’s potential exoplanetary system are possible with relatively cheap instrumentation. Authors studying habitability in this system typically adopt habitable zones (HZs) based on global radiative balance models that neglect the radiative perturbations of α Cen A.

We investigate the habitability of planets around α Cen B using one-dimensional latitudinal energy balance models (LEBMs), which fully incorporate the presence of α Cen A as a means of astronomically forcing terrestrial planet climates. We find that the extent of the HZ is relatively unchanged by the presence of α Cen A, but there are variations in fractional habitability for planets orbiting at the boundaries of the zone due to α Cen A, even in the case of zero eccentricity. Temperature oscillations of a few K can be observed at all planetary orbits, the strength of which varies with the planet’s ocean fraction and obliquity.