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We present Atacama Large Millimeter/submillimeter Array (ALMA) observationsof a protoplanetary disk around the T Tauri star Sz~84 and analyses of thestructures of the inner cavity in the central region of the dust disk. Sz~84'sspectral energy distribution (SED) has been known to exhibit negligibleinfrared excess at $\lambda \lesssim$10~$\mu$m due to the disk's cavitystructure. Analyses of the observed visibilities of dust continuum at 1.3~mmand the SED indicate that the size of the cavity in the disk of large(millimeter size) dust grains is 8~au in radius and that in the disk of small(sub-micron size) dust grains is 60~au in radius. Furthermore, from the SEDanalyses, we estimate that the upper limit mass of small dust grains at$r<$60~au is less than $\sim$10$^{-3}$~$M_{\rm earth}$, which is$\lesssim$0.01~\% of the total (small~$+$~large) dust mass at $r<$60~au. Theseresults suggest that large dust grains are dominant at $r<$60~au, implying thatdust grains efficiently grow with less efficient fragmentation in this region,potentially due to weak turbulence and/or stickier dust grains. The balance ofgrain growth and dust fragmentation is an important factor for determining thesize of large dust grains in protoplanetary disks, and thus Sz~84 could serveas a good testbed for investigations of grain growth in such disks.

ALMA Observations of the Inner Cavity in the Protoplanetary Disk around Sz 84