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Results: We found that the (B-V) v.s. (V-S9W) color-color diagram is usefulto identify the stars with infrared excess emerged from circumstellarenvelopes/disks. Be stars with infrared excess are well separated from othertypes of stars in this diagram. Whereas (J-L18W) v.s. (S9W-L18W) diagram is apowerful tool to classify several object-types. Carbon-rich asymptotic giantbranch (AGB) stars and OH/IR stars form distinct sequences in this color-colordiagram. Young stellar objects (YSOs), pre-main sequence (PMS) stars, post-AGBstars and planetary nebulae (PNe) have largest mid-infrared color-excess, andcan be identified in infrared catalog. Finally, we plot L18W v.s. (S9W-L18W)color-magnitude diagram, using the AKARI data together with Hipparcosparallaxes. This diagram can be used to identify low-mass YSOs, as well as AGBstars. We found that this diagram is comparable to the [24] vs ([8.0]-[24])diagram of Large Magellanic Cloud sources using the Spitzer Space Telescopedata. Our understanding of Galactic objects will be used to interpretcolor-magnitude diagram of stellar populations in nearby galaxies which SpitzerSpace Telescope has observed.  Conclusions: Our study of the AKARI color-color and color-magnitude will beused to explore properties of unknown objects in future. In addition, ouranalysis highlights a future key project to understand stellar evolution withcircumstellar envelope, once the forthcoming astronometrical data with GAIA areavailable.

AKARI's infrared view on nearby stars : Using AKARI Infrared Camera All-Sky Survey, 2MASS, and Hipparcos catalog