Clara Hung (Summit K2 High School / ASIAA); Po-Sheng Ou (ASIAA / NTU); You-Hua Chu (ASIAA); Robert A. Gruendl (UIUC); Chuan-Jui Li (ASIAA)
Wolf Rayet (WR) stars are evolved massive stars known to produce fast stellar winds between 1000 - 3000 km/s. These winds interact with the ambient medium to form shell structures, which, indeed, have been observed. However, the stellar wind interactions begin as early as the star’s Main Sequence stage when fast winds sweep up the interstellar medium (ISM) to form an interstellar bubble (ISB). As the star evolves into a red supergiant (RSG) or luminous blue variable (LBV), it ejects stellar material through slow winds to form a circumstellar nebula. When the star enters the WR stage, the fast stellar wind sweeps up the ambient circumstellar nebula to form a circumstellar bubble (CSB). In order to study the interaction of these structures with the ambient medium, we must first acquire a thorough understanding of the interstellar environment the WR star is in. To date, surveys of WR stars in the Large Magellanic Cloud (LMC) have produced a fairly complete catalog of 154 known stars. With new surveys of neutral and ionized gas and these known WR stars, we are able to conduct a comprehensive, multi-wavelength study of the multi-phase interstellar environment of WR stars for the first time. Specifically, we examined the Magellanic Cloud Emission Line Survey (MCELS) images in the H-alpha, [O III], and [S II] lines, Spitzer IRAC 8 micron images and MIPS 24 micron images, and 4m MOSAIC H-alpha images for the entire LMC. This allows us to examine the WR stars and their associated nebulae more extensively. In this poster we report our methodology and results on the morphology and statistics of the nebular structures of WR stars and their implications on stellar evolution.