![]() ![]() Finally, I demonstrate the immense potential of using asteroseismology to probe the interiors of evolved massive stars, and discover a new class of pulsating supergiant. However, these methods can only be used given large numbers of well-classified stars, and I show that even using advanced machine learning techniques, existing data are insufficient to classify these stars. My studies of populations of young stars reveal that the massive star binary fraction can be inferred using only simple demographic statistics. These fusion reactions create new atomic nuclei. Not only do stars go through a life cycle, but they are also. As a massive star collapses, it produces a shockwave that can induce fusion reactions in the stars outer shell. Combined with chemical compositions, mass determines a stars luminosity, its physical size. ![]() These giants are typically found in the densely populated hearts of dust-shrouded star clusters. One big obstacle standing in the way of scientists trying to solve this puzzle is obtaining observations of these stars. In this work, I attempt to understand evolved massive stars using a variety of techniques that have only recently begun to be applied to these interesting objects. Massive stars are classified by having a solar mass that is eight times the size of the sun during its main sequence life cycle stage. Stellar mass is the most important attribute of a star. Astronomers still do not understand how massive stars, which are more than 100 times the mass of the Sun, are formed. Due to their rarity, these multitudinous unknowns remain under-constrained. ![]() Individually, they are fascinating astrophysical laboratories in which many of the unknowns of stellar evolution coalesce. As residents of their host galaxies, they inject radiation and matter into their surroundings on short timescales before exploding as supernovae. Evolved massive stars - the post-main sequence descendants of stars with initial masses higher than roughly 8 solar masses - are rare yet critically important objects. Despite high mass stars (> 8 M) are more scarce than their lower-mass counterparts, they play an important role in many respects. ![]()
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