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The LAMOST spectra and $\it{Kepler}$ light curves are combined to investigatethe detached eclipsing binary KIC 8098300, which shows the O'Connell effectcaused by spot/facula modulation. The radial velocity (RV) measurements arederived by using the tomographic spectra disentangling technology. The massratio $q = K_1/K_2 = 0.812 \pm 0.007$, and the orbital semi-major axis$a\mathrm{\sin}i = 14.984 \pm 0.048\ R_\odot$ are obtained by fitting the RVcurves. We optimize the binary model concerning the spot/facula activity withthe code PHOEBE and obtain precise parameters of the orbit including theeccentricity $e=0.0217 \pm 0.0008$, the inclination $i=87.71\pm 0.04^\circ$,and the angle of periastron $\omega=284.1\pm 0.5^\circ$. The masses and radiiof the primary and secondary star are determined as $M_1=1.3467 \pm 0.0001\M_\odot$, $R_1=1.569 \pm 0.003\ R_\odot$, and $M_2=1.0940 \pm 0.0001\ M_\odot$,$R_2=1.078 \pm 0.002\ R_\odot$, respectively. The ratio of temperatures of thetwo component stars is $r_{teff}=0.924 \pm 0.001$. We also obtain theperiastron precession speed of $0.000024\pm 0.1\ \mathrm{d}\ cycle^{-1}$.The residuals of out-of-eclipse are analyzed using the Auto-CorrelationFunction (ACF) and the Discrete Fourier Transform (DFT). The spot/faculaactivity is relatively weaker, but the lifetime is longer than that of mostsingle main sequence stars in the same temperature range. The average rotationperiod of the spots $P_{rot}=4.32\ d$ is slightly longer than the orbitalperiod, which may be caused by either the migration of spots/faculae along thelongitude or the latitudinal differential rotation. The activity may bespot-dominated for the secondary star and facula-dominated for the primarystar.

Spot and Facula Activity Variations of the Eccentric Detached Eclipsing Binary KIC 8098300 Based on the Time-series Orbital Solutions