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In this study, a W Ursae Majoris (W UMa) type system LO Andromedae (LO And)was observed over nine nights at Durham to fully investigate its physicalproperties and update its stellar parameters. After obtaining the observationaldata in both V-filter and B-filter, the Gaia CCD images of LO And wereextracted from the Astrolab internal archive using Linux commands. By applyingthe "Nightfall" program and local Python scripts, the calibrated light curvesof LO And can be plotted, phase-folded, and fitted to derive the period of thissystem as $0.3804573 \pm 0.0000482\, \mathrm{d}$. Then, 2D chi-squared heatmaps were illustrated to determine LO And's best-fit stellar parameters andestimate their uncertainties, including the mass ratio $q = 0.371 \pm 0.207$,the inclination $i = 78.5 \pm 3.8\, \mathrm{deg}$, the primary temperature $T_1= 6290 \pm 358\, \mathrm{K}$, the secondary temperature $T_2 = 6449 \pm 445\,\mathrm{K}$, and two fill factors $f_1 = f_2 = 1.02258$. In addition, the"Nightfall" program built the 3D models and evaluated the spot distributionparameters to visualize the configuration of LO And. There were seven neweclipsing timings added in this study to reconstruct the O-C diagram togetherwith LO And's previous observational data. It was clearly found that the periodof LO And is currently undergoing an accelerated increase with a change rate$d\mathrm{P}/d\mathrm{t} = 2.27 \times 10^{-7}\, \mathrm{day\, yr^{-1}}$, whichwas attributed to the mass transfer in this system with a transfer rate$dM_1/d\mathrm{t} = 1.43 \times 10^{-7}\, \mathrm{M_\odot\, yr^{-1}}$ and thelight time effect caused by the possible existence of a third star $M_3 =0.224\, M_\odot$ orbiting around LO And.

A new investigation on the characteristics of a W UMa type system LO Andromedae