High-energy cosmic rays from all directions in space enter the Earth’s atmosphere. Interaction of
these cosmic rays in the atmosphere produces secondary particles, including neutrinos. Generally
the behavior of atmospheric neutrino flux is accepted as a power-law function type, although the
shape varies at different energies and zenith angles. Due to these complications, the fluxes from
detailed numerical calculations are reported in energy and zenith angle bins. In this article we
propose new interpolation schemes for the flux in energy bins or energy and zenith angle bins
for any power-law type function. We apply these schemes to the atmospheric muon neutrino flux
model H3a QGSJET-II-4.