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After the sunspot maximum and the reversal of solar polarity in 2014, the Sun is now in the early declining phase of cycle 24. Soon after the polarity reversa l, the galactic cosmic ray intensity, as observed, e.g., by neutron monitors at several latitudes (c ut-off rigidities) depict an exceptionally large variation at the solar rotation period. This recurren ce started in mid-2014 and continues until now (the first half of March 2015). Several parameters charac te izing solar activity, like sunspots and F10.7 radio flux, also depict similar enhanced variabili ty, which started slightly earlier than in neutron monitors. Some solar wind properties also show th is periodicity, although less systematically and for a shorter time. This excessively strong per iodicity in GCR can be related to the rapid growth of an asymmetric polar coronal hole in the south ern hemisphere, leading to a very asymmetric magnetic configuration at midto high heliosphe ric latitudes. This also leads to the fact that the tilt angle of the heliospheric current sheet is more changeable, during this cycle than at similar early declining phases of the previous solar cycl es.

Exceptionally strong variation of galactic cosmic ray intensity at solar rotation period after the maximum of solar cycle 2