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We construct a numerical model of steady-state, general relativistic (GR)super-Eddington accretion flows in an optically thick, advection-dominatedregime, motivated by tidal disruption events wherein super-Eddington accretionassumes a pivotal role. Our model takes into account the loss of angularmomentum due to radiation and the scale-height derivative in the basicequations of the GR slim disk. For comparison purposes, we also provide a newanalytical solution for a radiation-pressure-dominant GR slim disk, whichneglects the angular momentum loss due to radiation and the scale-heightderivative. We find that the radiation pressure enhances by incorporating thescale height derivative into the basic equations. As a result, the surfacedensity near the disk's inner edge decreases, whereas the disk temperature andscale height increase, brightening the disk spectrum in the soft X-raywaveband. Notably, an extremely high mass accretion rate significantly enhancesthe effect of the scale-height derivative, affecting the entire disk. Incontrast, the inclusion of the radiation-driven angular momentum loss onlyslightly influences the disk surface density and temperature compared with thecase of the scale-height derivative inclusion. The X-ray luminosity increasessignificantly due to scale height derivative for $\dot{M}/\dot{M}_{\rm Edd}\gtrsim 2$. In addition, the increment is higher for the non-spinning blackhole than the spinning black hole case, resulting in a one-order of magnitudedifference for $\dot{M}/\dot{M}_{\rm Edd}\gtrsim100$. We conclude thatincorporating the scale-height derivative into a GR slim disk model is crucialas it impacts the disk structure and its resultant spectrum, particularly on asoft-X-ray waveband.

Impact of scale-height derivative on general relativistic slim disks in tidal disruption events