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We study the cosmic ray arrival distribution expected from a source ofneutrons in the galactic center at energies around 1 EeV and compare it withthe anisotropy detected by AGASA and SUGAR. Besides the point-like signal inthe source direction produced by the direct neutrons, an extended signal due tothe protons produced in neutron decays is expected. This associated protonsignal also leads to an excess in the direction of the spiral arm. Forrealistic models of the regular and random galactic magnetic fields, theresulting anisotropy as a function of the energy is obtained. We find that forthe anisotropy to become sufficiently suppressed below E\sim 10^{17.9}eV, asignificant random magnetic field component is required, while on the otherhand, this also tends to increase the angular spread of the associated protonsignal and to reduce the excess in the spiral arm direction. The sourceluminosity required in order that the right ascension anisotropy be 4% for theAGASA angular exposure corresponds to a prediction for the point-like flux fromdirect neutrons compatible with the flux detected by SUGAR. We also analyse thedistinguishing features predicted for a large statistics southern observatory.Comment: 14 pages, 6 figures, minor changes to match published versio

Decaying neutron propagation in the galaxy and the cosmic ray anisotropy at 1 EeV