  The behaviour of the large-scale dipolar field, during a star's magnetic
cycle, can provide valuable insight into the stellar dynamo and associated
magnetic field manifestations such as stellar winds. We investigate the
temporal evolution of the dipolar field of the K dwarf 61 Cyg A using
spectropolarimetric observations covering nearly one magnetic cycle equivalent
to two chromospheric activity cycles. The large-scale magnetic field geometry
is reconstructed using Zeeman Doppler imaging, a tomographic inversion
technique. Additionally, the chromospheric activity is also monitored. The
observations provide an unprecedented sampling of the large-scale field over a
single magnetic cycle of a star other than the Sun. Our results show that 61
Cyg A has a dominant dipolar geometry except at chromospheric activity maximum.
The dipole axis migrates from the southern to the northern hemisphere during
the magnetic cycle. It is located at higher latitudes at chromospheric activity
cycle minimum and at middle latitudes during cycle maximum. The dipole is
strongest at activity cycle minimum and much weaker at activity cycle maximum.
The behaviour of the large-scale dipolar field during the magnetic cycle
resembles the solar magnetic cycle. Our results are further confirmation that
61 Cyg A indeed has a large-scale magnetic geometry that is comparable to the
Sun's, despite being a slightly older and cooler K dwarf.
