Prospects for directly detecting the first supernovae, and their impact on early star formation

dc.contributor.advisorBromm, Volkeren
dc.contributor.committeeMemberMilosavljevic, Milosen
dc.contributor.committeeMemberWheeler, J. Craigen
dc.contributor.committeeMemberFinkelstein, Stevenen
dc.contributor.committeeMemberYoshida, Naokien
dc.creatorHummel, Jacob Alexanderen
dc.creator.orcid0000-0001-8423-1225en 2016
dc.description.abstractThe formation of the first stars in the Universe marked a pivotal moment in cosmic history, initiating the transition from the simple initial conditions of the big bang to the complex structures we see today. Ionizing radiation produced by these so-called Population III stars began the process of reionization, and the supernovae marking their deaths initiated the process of chemical enrichment. We assess the prospects for direct detection of the first supernovae should they happen to end their lives as extremely energetic pair-instability supernovae, which should be within the detection limits of the upcoming James Webb Space Telescope. Using a combination of semi-analytic models and cosmological simulations to estimate their source density, we find that the primary obstacle to observing such events is their scarcity, not their faintness. The first supernovae and the compact remnants they leave behind also produce significant amounts of high-energy X-rays and cosmic rays able to travel through the predominantly neutral intergalactic medium and build up a cosmic background. To better understand how these violent explosions impact subsequent episodes of metal-free star formation, we employ ab-initio, cosmological hydrodynamics simulations to model the formation of stars in a minihalo at z = 20-30 under the influence of both an X-ray and cosmic ray background. The presence of an ionizing background---whether X-rays or cosmic rays---serves to expedite the collapse of gas to high densities by enhancing molecular hydrogen cooling, thus allowing stars to form at substantially earlier epochs in strongly irradiated minihalos. The mass of the stars thus formed however appears to be quite robust, maintaining a characteristic mass of order a few tens of solar masses even as the strength of the ionizing background varies by several orders of magnitude. Finally, we describe the novel software developed to enable this research. These tools for manipulating and analyzing simulation data have been released as the open-source GAdget DataFrame Library: gadfly.en
dc.subjectFirst starsen
dc.subjectStar formationen
dc.titleProspects for directly detecting the first supernovae, and their impact on early star formationen
dc.type.materialtexten University of Texas at Austinen of Philosophyen

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