HARPS and Kepler results indicate that half of solar-type stars host planets with periods P < 100 d and masses M < 30 M _ { \oplus } .
These super Earth systems are compact and dynamically cold .
Here we investigate the stability of the super Earth system around the K-dwarf HD40307 .
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 3.1 \sigma 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 black-body 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 3 d. A rotation period of about 1.5 d could cause extreme obliquity variations because of capture in a Cassini state .
For faster rotation rates the periods converge to 10 kyr and 20 kyr .
The large uncertainty in the precession period does not change the overall outcome .