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XTE J1946+274 is a Be/X-ray binary with a 15.8s spin period and 172 d orbitalperiod. Using $\textit{RXTE/PCA}$ data of the 1998 outburst, a cyclotron linearound 37 keV was reported. The presence of this line, its dependence on thepulse 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 theother during the declining phase of the 2021 outburst. We also present a newanalysis of the $\textit{Insight}$-HXMT observations of the source at the peakof the 2018 outburst. We find the source to be spinning up over the course ofthe outburst and spinning down between the two outbursts. We report thepresence 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 the2021 outburst using data from $\textit{AstroSat}$. We also investigate thepulse phase dependence of the cyclotron line parameters and find that the lineis significantly detected in all the phases of both $\textit{AstroSat}$observations, along with showing variation with the pulse phase. This differsfrom the previous results reported using $\textit{BeppoSAX}$ and$\textit{NuSTAR}$. We explain this behaviour of the cyclotron line to be due tophoton spawning and different accretion column radii at the two poles of thisneutron star.

$\textit{Insights}$ into the phase-dependent cyclotron line feature in XTE J1946+274: An $\textit{AstroSat}$ and $\textit{Insight}$-HXMT view