2014MNRAS.440.3685B

HARPS and Kepler results indicate that half of solar-type stars host planets with periods P < 100d and masses M < 30 M⊕. These super-Earth systems are compact and dynamically cold. Here, we investigate the stability of the super-Earth system around the K-dwarf HD 40307. It could host up to six planets, with one in the habitable zone. We analyse the system's stability using numerical simulations from initial conditions within the observational uncertainties. The most stable solution deviates 3.1σ from the published value, with planets e and f not in resonance and planets b and c apsidally aligned. We study the habitability of the outer planet through the yearly averaged insolation and blackbody temperature at the pole. Both undergo large variations because of its high eccentricity and are much more intense than on Earth. The insolation variations are precession dominated with periods of 40 kyr and 10² kyr for precession and obliquity if the rotation period is 3d. A rotation period of about 1.5d could cause extreme obliquity variations because of capture in a Cassini state. For faster rotation rates, the periods converge to 10 and 20 kyr. The large uncertainty in the precession period does not change the overall outcome.