SUMMARY AND CONCLUSIONS

The H-R diagram method seemed to make the most sense, due to the plotted stars’ agreement with the curvature of the Hayashi tracks. Also, this method seems to depend much less on data that could change with such variable stars. This data also relied on photometric data that was de-reddened, which compensates for obscuring gas and dust.
When plotting the degree of emissivity versus the absolute magnitude, a linear correlation is found. This means that as a star becomes less emissive, it becomes brighter. This can mean two things: that more massive stars emit less, or that as a star is less emissive, the gas and dust around it dissipates, so one can see more of the star, and thus it brightens.
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