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We investigate the relation between the spatiotemporal evolution of thedimming region and the dominant direction of the filament eruption and CMEpropagation for the 28 October 2021 X1.0 flare/CME event observed from multipleviewpoints by Solar Orbiter, STEREO-A, SDO, and SOHO. We propose a method toestimate the dominant dimming direction by tracking its area evolution andemphasize its accurate estimation by calculating the surface area of a spherefor each pixel. To determine the early flux rope propagation direction, weperform 3D reconstruction of the CME via graduated cylindrical shell modeling(GCS) and tie-pointing of the filament. The dimming initially expands radiallyand later shifts southeast. The orthogonal projections of the reconstructedheight evolution of the erupting filament onto the solar surface are located inthe sector of the dominant dimming growth, while the orthogonal projections ofthe inner part of GCS reconstruction align with the total dimming area. Thefilament reaches a maximum speed of $\approx$250 km/s at a height of about$\approx$180 Mm. The direction of its motion is strongly inclined from theradial (64$^\circ$ to the East, 32$^\circ$ to the South). The 50$^\circ$difference in the 3D direction between the CME and the filament leg closelycorresponds to the CME half-width determined from reconstruction, suggesting apotential relation of the reconstructed filament to the associated leg of theCME body. Our findings highlight that the dominant propagation of the dimminggrowth reflects the direction of the erupting magnetic structure (filament) lowin the solar atmosphere, though the filament evolution is not related directlyto the direction of the global CME expansion. The overall dimming morphologyclosely resembles the inner part of the CME reconstruction, validating the useof dimming observations to obtain insight into the CME direction.

On the three-dimensional relation between the coronal dimming, erupting filament and CME. Case study of the 28 October 2021 X1.0 event