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We present MeerKAT Fornax Survey atomic hydrogen (HI) observations of thedwarf galaxies located in the central ~2.5 x 4 deg$^2$ of the Fornax galaxycluster. The HI images presented in this work have a $3\sigma$ column densitysensitivity between 2.7 and 50 x 10$^{18}$ cm$^{-2}$ over 25 km s$^{-1}$ forspatial resolution between 4 and 1 kpc. We are able to detect an impressive MHI= 5 x 10$^{5}$ Msun 3$\sigma$ point source with a line width of 50 km s$^{-1}$at a distance of 20 Mpc. We detect HI in 17 out of the 304 dwarfs in our field-- 14 out of the 36 late type dwarfs (LTDs), and 3 of the 268 early type dwarfs(ETDs). The HI-detected LTDs have likely just joined the cluster and are ontheir first infall as they are located at large clustocentric radii, withcomparable MHI and mean stellar surface brightness at fixed luminosity as blue,star-forming LTDs in the field. The HI-detected ETDs have likely been in thecluster longer than the LTDs and acquired their HI through a recent merger oraccretion from nearby HI. Eight of the HI-detected LTDs host irregular orasymmetric HI emission and disturbed or lopsided stellar emission. There aretwo clear cases of ram-pressure shaping the HI, with the LTDs displayingcompressed HI on the side closest to the cluster centre and a one-sided,starless tail pointing away from the cluster centre. The HI-detected dwarfsavoid the most massive potentials, consistent with massive galaxies playing anactive role in the removal of HI. We create a simple toy model to quantify thetimescale of HI stripping in the cluster. We find that a MHI = 10$^{8}$ Msundwarf will be stripped in ~ 240 Myr. The model is consistent with ourobservations, where low mass LTDs are directly stripped of their HI from asingle encounter and more massive LTDs can harbour a disturbed HI morphologydue to longer times or multiple encounters being required to fully strip theirHI.

The MeerKAT Fornax Survey II. The rapid removal of HI from dwarf galaxies in the Fornax cluster