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We present the results of the X-ray flaring activity of 1ES 1959+650 duringOctober 25-26, 2017 using AstroSat observations. The source was variable in theX-ray. We investigated the evolution of the X-ray spectral properties of thesource by dividing the total observation period ($\sim 130$ ksecs) into timesegments of 5 ksecs, and fitting the SXT and LAXPC spectra for each segment.Synchrotron emission of a broken power-law particle density model provided abetter fit than the log-parabola one. The X-ray flux and the normalisedparticle density at an energy less than the break one, were found toanti-correlate with the index before the break. However, a stronger correlationbetween the density and index was obtained when a delay of $\sim 60$ ksec wasintroduced. The amplitude of the normalised particle density variation $|\Deltan_\gamma/n_\gamma| \sim 0.1$ was found to be less than that of the index$\Delta \Gamma \sim 0.5$. We model the amplitudes and the time delay in ascenario where the particle acceleration time-scale varies on a time-scalecomparable to itself. In this framework, the rest frame acceleration time-scaleis estimated to be $\sim 1.97\times10^{5}$ secs and the emission region size tobe $\sim 6.73\times 10^{15}$ cms.

AstroSat observation of the HBL 1ES 1959+650 during its October 2017 flaring