  In strong stellar and solar flares flare loops typically appear during the
decay phase, providing an additional contribution to the flare emission and,
possibly, obscuring the flare emission. Super-flares, common in active, cool
stars, persist mostly from minutes to several hours and alter the star's
luminosity across the electromagnetic spectrum. Recent observations of a young
main-sequence star reveal a distinctive cool loop arcade forming above the
flaring region during a 27-hour superflare event, obscuring the region multiple
times. Analysis of these occultations enables the estimation of the arcade's
geometry and physical properties. The arcade's size expanded from 0.213 to
0.391 R$_*$ at a speed of approximately 3.5$\,$km/s. The covering structure
exhibited a thickness below 12$\,$200$\,$km, with electron densities ranging
from 10$^{13}$ to 10$^{14}\,$cm$^{-3}$ and temperatures below 7$\,$600$\,$K,
6$\,$400$\,$K, and 5$\,$077$\,$K for successive occultations. Additionally, the
flare's maximum emission temperature has to exceed 12$\,$000$\,$K for the
occultations to appear. Comparing these parameters with known values from other
stars and the Sun suggests the structure's nature as an arcade of cool flare
loops. For the first time, we present the physical parameters and the
reconstructed geometry of the cool flare loops that obscure the flaring region
during the gradual phase of a long-duration flare on a star other than the Sun.
