AstroSat View of Transient Low-mass X-ray Binary XTE J1701-462: Spectral and Temporal Evolution along the Z-track

AstroSat observed transient neutron star low-mass X-ray binary XTE J1701-462 for a total duration of 135 ks during its 2022 outburst. The source traced a complete 'Z' shaped structure in the hardness intensity diagram (HID) during the observation. The source exhibited an extended horizontal branch and a short-dipping flaring branch in the HID. We find that most suitable spectral model comprises emission from a standard multi-color accretion disk and Comptonized radiation from a hot central corona. The observed disk component is cool having temperature in the range of 0.3-0.4 keV and truncated far ( ~100 - 520 km) from the compact object. The Compton corona has optical depth in the range of 3.3-5 and temperature in the range of 3.3-4.9 keV. The disk and corona flux as well as truncation radius varies significantly along the HID. We discuss the possible scenarios to explain the relationship between spectral evolution and motion of the source along the HID. The timing analysis revealed horizontal branch oscillations (HBOs) in the frequency range 34-60 Hz. The frequency and rms strength of HBO vary systematically as the source moves along the horizontal branch (HB). The observed correlation of HBO properties with the position on the HB is similar to that reported previously in this source using \textit{RXTE} data during the 2006 outburst of the source. The source also showed NBOs with frequency $\sim$ 6.7 Hz in the middle and lower normal branch. The energy dependent study of the HBO properties suggests that the HBO is stronger in the higher energy band. We also observed very-low frequency noise (VLFN) and band limited noise (BLN) components in the power-density spectra. The break frequency of BLN component was found to be tightly correlated with the HBO frequency. We discuss possible models to explain the origin and nature of the observed features in the PDS.