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V405 And is an ultrafast-rotating (P_rot ~ 0.46 days) eclipsing binary. Thesystem consists of a primary star with radiative core and convective envelope,and a fully convective secondary. Theories have shown, that stellar structurecan depend on magnetic activity, i.e., magnetically active M-dwarfs should havelarger radii. Earlier light curve modelling of V405 And indeed showed thisbehaviour: we found that the radius of the primary is significantly larger thanthe theoretically predicted value for inactive main sequence stars (thediscrepancy is the largest of all known objects), while the secondary fits wellto the mass-radius relation. By modelling our recently obtained light curves,which show significant changes of the spotted surface of the primary, we canfind further proof for this phenomenon.

Modelling of an eclipsing RS CVn-binary: V405 And