We present various infrared two-color diagrams (2CDs) using WISE data for asymptotic giant branch (AGB) stars and Planetary Nebulae (PNe) and investigate possible evolutionary tracks. We use the sample of 5036 AGB stars, 660 post-AGB stars, and 2748 PNe in our Galaxy. For each object, we cross-identify the IRAS, AKARI, WISE, and 2MASS counterparts. To investigate the spectral evolution from AGB stars to PNe, we compare the theoretical model tracks of AGB stars and post-AGB stars with the observations on the IR 2CDs. We find that the theoretical dust shell model tracks can roughly explain the observations of AGB stars, post-AGB stars, and PNe on the various IR 2CDs. WISE data are useful in studying the evolution of AGB stars and PNe, especially for dim objects. We find that most observed color indices generally increase during the evolution from AGB stars to PNe. We also find that Fe0.9Mg0.1O dust is useful to fit the observed WISE W3-W4 colors for O-rich AGB stars with thin dust shells.

Abstract
1. INTRODUCTION
2. SAMPLE STARS
    2.1. Infrared Photometric Data
    2.2. Counterparts for IRAS PSC sources
    2.3. AGB stars
    2.4. Post-AGB stars
    2.5. Planetary Nebulae
3. INFRARED TWO-COLOR DIAGRAMS
4. THEORETICAL DUST SHELL MODELS
    4.1. Dust Shell Models for AGB Stars
    4.2. Dust Shell Models for Post-AGB Stars
5. COMPARISON BETWEEN THEORY ANDOBSERVATIONS
    5.1. Limitations of the TheoreticalModels
    5.2. [25]-[60] versus [12]-[25]
    5.3. W3-W4 versusW2-W3
    5.4. [9]-[12] versus [12]-[25]
    5.5. W3-W4 versus K-W3
    5.6. Discussion of Fe 0.9Mg 0.1O and Alumina Dust
6. SUMMARY
REFERENCES

• Kyung-Won Suh(Department of Astronomy and Space Science, Chungbuk National University) Corresponding author