  We report the results obtained from a detailed timing and spectral studies of
Be/X-ray binary pulsar 2S 1417-624 using data from Swift and NuSTAR
observatories. The observations were carried out at the peak of a giant
outburst of the pulsar in 2018. X-ray pulsations at 17.475 s were detected in
the source light curves up to ~79 keV. The evolution of the pulse profiles with
energy was found to be complex. A four-peaked profile at lower energies
gradually evolved into a double-peak structure at higher energies. The pulsed
fraction of the pulsar, calculated from the NuSTAR observation was found to
follow an anti-correlation trend with luminosity as observed during previous
giant X-ray outburst studies in 2009. The broadband spectrum of the pulsar is
well described by a composite model consisting of a cutoff power law model
modified with the interstellar absorption, a thermal blackbody component with a
temperature of $\approx$1 keV and a Gaussian function for the 6.4 keV iron
emission line. Though the pulsar was observed at the peak of the giant
outburst, there was no signature of presence of any cyclotron line feature in
the spectrum. The radius of the blackbody emitting region was estimated to be
$\approx$2 km, suggesting that the most probable site of its origin is the
stellar surface of the neutron star. Physical models were also explored to
understand the emission geometry of the pulsar and are discussed in the paper.
