  We present the near- to mid-infared study of supernova remnants (SNRs) using
the AKARI IRC Survey of the Large Magellanic Cloud (LMC). The LMC survey
observed about a 10 square degree area of the LMC in five bands centered at 3,
7, 11, 15, and 24 \micron using the Infrared Camera (IRC) aboard AKARI. The
number of SNRs in the survey area is 21, which is about a half of the known LMC
SNRs. We systematically examined the AKARI images and identified eight SNRs
with distinguishable infrared emission. All of them were detected at $\gtrsim
10$ \micron and some at 3 and 7 \micron, too. We present their AKARI images and
fluxes. In the 11/15 \micron versus 15/24 \micron color-color diagram, the SNRs
appear to be aligned along a modified blackbody curve, representing thermal
emission from dust at temperatures between 90 and 190 K. There is a good
correlation between the 24 \micron and X-ray fluxes of the SNRs. It was also
found that there is a good correlation between the 24 \micron and radio fluxes
even if there is no direct physical connection between them. We considered the
origin of the detected mid-infrared emission in individual SNRs. We conclude
that the mid-infrared emissions in five SNRs that show morphologies similar to
the X-rays are dominated by thermal emission from hot dust heated by X-ray
emitting plasma. Their 15/24 \micron color temperatures are generally higher
than the Spitzer 24/70 \micron color temperatures, which suggests that a
single-temperature dust model cannot describe the full spectral energy
distribution (SED) of the SNRs. It also implies that our understanding of the
full SED is essential for estimating the dust destruction rate of grains by SNR
shocks.
