  XTE J1946+274 is a Be/X-ray binary with a 15.8s spin period and 172 d orbital
period. Using $\textit{RXTE/PCA}$ data of the 1998 outburst, a cyclotron line
around 37 keV was reported. The presence of this line, its dependence on the
pulse phase, and its variation with luminosity have been of some debate since.
In this work, we present the reanalysis of two $\textit{AstroSat}$
observations: one made during the rising phase of the 2018 outburst and the
other during the declining phase of the 2021 outburst. We also present a new
analysis of the $\textit{Insight}$-HXMT observations of the source at the peak
of the 2018 outburst. We find the source to be spinning up over the course of
the outburst and spinning down between the two outbursts. We report the
presence of a higher cyclotron line energy using the 2018 $\textit{AstroSat}$
observation ($\sim 45$ keV) and 2018 $\textit{Insight}$-HXMT observation
($\sim$ 50 keV) and a line at $\sim$ 40 keV during the declining phase of the
2021 outburst using data from $\textit{AstroSat}$. We also investigate the
pulse phase dependence of the cyclotron line parameters and find that the line
is significantly detected in all the phases of both $\textit{AstroSat}$
observations, along with showing variation with the pulse phase. This differs
from the previous results reported using $\textit{BeppoSAX}$ and
$\textit{NuSTAR}$. We explain this behaviour of the cyclotron line to be due to
photon spawning and different accretion column radii at the two poles of this
neutron star.
