INTRODUCTION

Young Stellar Objects (YSOs) are variable stars of about ten million years of age and rapidly fluctuate with temperature, spectral type, wind outflows and inflows and magnitude. Some also have spectral anomalies which may indicate the presence of circum-stellar dust. Spectral types of these stars range from B type to K and they have irregular periods, varying by up to four magnitudes. They have associated nebulosity where changes have been observed over the years. On the H-R Diagram, they are on one of the Hayashi Tracks, leading into the main sequence. The goal of this study is that by studying these stars’ spectra, imaging data, and photometric data, these stars can be placed more precisely into the evolutionary tracks of young stars. A secondary goal is to gain insight into possible mechanisms that explain the peculiar chemistries and changes in YSOs.
Four types of YSOs were observed: T Tauri, FU Orionis, Variable Stars of Orionis (VSOs) type, and Herbig Ae/Be stars. T Tauri and FU Orionis stars are three or less solar masses, but FU Orionis are more eruptive. Herbig Ae/Be stars are of four to eight solar masses. YSOs represent the earlier spectral classes such as B and A type. As with all stars at this stage of evolution, nuclear fusion is not sustained, thus outflows, magnitude, temperature, and many other aspects vary.
The main purpose of the project was to observe many types of Young Stellar Objects, such as T Tauri stars and Herbig Ae/Be stars, to compare the effectiveness of several methods of calculating relative age.
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