  We investigate the properties of plasmoids observed in the current sheet
formed after an X-8.3 flare followed by a fast CME eruption on September 10,
2017 using Extreme Ultraviolet (EUV) and white-light coronagraph images. The
main aim is to understand the evolution of plasmoids at different
spatio-temporal scales using existing ground- and space-based instruments. We
identified the plasmoids in current sheet observed in the successive images of
{\it Atmospheric Imaging Assembly} (AIA) and white-light coronagraphs, K-Cor
and LASCO/C2. We found that the current sheet is accompanied by several
plasmoids moving upwards and downwards. Our analysis showed that the downward
and upward moving plasmoids have average width of 5.92 Mm and 5.65 Mm,
respectively in the AIA field of view (FOV). However, upward moving plasmoids
have average width of 64 Mm in the K-Cor which evolves to a mean width of 510
Mm in the LASCO/C2 FOV. Upon tracking the plasmoids in successive images, we
observe that downward and upward moving plasmoids have average speeds of
$\sim$272 km s$^{-1}$ and $\sim$191 km s$^{-1}$ respectively in the EUV
passbands. We note that the plasmoids become super-Alfv\'enic when they reach
at LASCO FOV. Furthermore, we estimate that the null-point of the current sheet
at $\approx$ 1.15 R$_\odot$ where bidirectional plasmoid motion is observed. We
study the width distribution of plasmoids formed and notice that it is governed
by a power law with a power index of -1.12. Unlike previous studies there is no
difference in trend for small and large scale plasmoids. The presence of
accelerating plasmoids near the neutral point indicates a longer diffusion
region as predicted by MHD models.
