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We report a new, plasmoid-fed scenario for the formation of an eruptiveprominence (PF$^2$), involving reconnection and condensation. We usegrid-adaptive resistive two-and-a-half-dimensional magnetohydrodynamic (MHD)simulations in a chromosphere-to-corona setup to resolve this plasmoid-fedscenario. We study a pre-existing flux rope (FR) in the low corona thatsuddenly erupts due to catastrophe, which also drives a fast shock above theerupting FR. A current sheet (CS) forms underneath the erupting FR, withchromospheric matter squeezed into it. The plasmoid instability occurs andmultiple magnetic islands appear in the CS once the Lundquist number reaches$\sim 3.5\times 10^{4}$. The remnant chromospheric matter in the CS is thentransferred to the FR by these newly formed magnetic islands. The dense andcool mass transported by the islands accumulates in the bottom of the FR,thereby forming a prominence during the eruption phase. More coronal plasmacontinuously condenses into the prominence due to the thermal instability asthe FR rises. Due to the fine structure brought in by the PF$^2$ process, themodel naturally forms filament threads, aligned above the polarity inversionline. Synthetic views at our resolution of $15 \mathrm{km}$ show many detailsthat may be verified in future high-resolution observations.

Plasmoid-fed prominence formation (PF$^2$) during flux rope eruption