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dc.creatorRitter, Jeremy S.en_US
dc.creatorSafranek-Shrader, Chalenceen_US
dc.creatorGnat, Orlyen_US
dc.creatorMilosavljevic, Milosen_US
dc.creatorBromm, Volkeren_US
dc.date.accessioned2016-04-28T19:41:55Z
dc.date.available2016-04-28T19:41:55Z
dc.date.issued2012-12en
dc.identifierdoi:10.15781/T2F82M
dc.identifier.citationRitter, Jeremy S., Chalence Safranek-Shrader, Orly Gnat, Miloレ Milosavljevi?, and Volker Bromm. "Confined Population III Enrichment and the Prospects for Prompt Second-generation Star Formation." The Astrophysical Journal, Vol. 761, No. 1 (Dec., 2012): 56.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/35125
dc.description.abstractIt is widely recognized that nucleosynthetic output of the first Population III supernovae was a catalyst defining the character of subsequent stellar generations. Most of the work on the earliest enrichment was carried out assuming that the first stars were extremely massive and that the associated supernovae were unusually energetic, enough to completely unbind the baryons in the host cosmic minihalo and disperse the synthesized metals into the intergalactic medium. Recent work, however, suggests that the first stars may in fact have been somewhat less massive, with a characteristic mass scale of a few tens of solar masses. We present a cosmological simulation following the transport of the metals synthesized in a Population III supernova assuming that it had an energy of 1051 erg, compatible with standard Type II supernovae. A young supernova remnant is inserted in the first star's relic H II region in the free expansion phase and is followed for 40 Myr employing adaptive mesh refinement and Lagrangian tracer particle techniques. The supernova remnant remains partially trapped within the minihalo, and the thin snowplow shell develops pronounced instability and fingering. Roughly half of the ejecta turn around and fall back toward the center of the halo, with 1% of the ejecta reaching the center in similar to 30 kyr and 10% in similar to 10 Myr. The average metallicity of the combined returning ejecta and the pristine filaments feeding into the halo center from the cosmic web is similar to 0.001-0.01 Z(circle dot), but the two remain unmixed until accreting onto the central hydrostatic core that is unresolved at the end of the simulation. We conclude that if Population III stars had less extreme masses, they promptly enriched the host minihalos with metals and triggered Population II star formation.en_US
dc.description.sponsorshipNSF AST-0708795, AST-1009928en_US
dc.description.sponsorshipNASA ATFP NNX09AJ33Gen_US
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectcosmology: theoryen_US
dc.subjectgalaxies: dwarfen_US
dc.subjectgalaxies: formationen_US
dc.subjecthydrodynamicsen_US
dc.subjectism: structureen_US
dc.subjectstars: formationen_US
dc.subjectsupernovae: generalen_US
dc.subjectinitial mass functionen_US
dc.subjectmetal-poor starsen_US
dc.subjectmilky-way satellitesen_US
dc.subjectcold-dark-matteren_US
dc.subjectultraviolet radiative feedbacken_US
dc.subjectpair-instabilityen_US
dc.subjectsupernovaeen_US
dc.subjectglobular-cluster formationen_US
dc.subjectsupermassive black-holesen_US
dc.subjectgianten_US
dc.subjectmolecular cloudsen_US
dc.subjectprimordial hii-regionsen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleConfined Population III Enrichment And The Prospects For Prompt Second-Generation Star Formationen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.Filename2012_12_confinedpopulationiii.pdfen_US
dc.rights.restrictionOpenen_US
dc.identifier.doi10.1088/0004-637x/761/1/56en_US
dc.contributor.utaustinauthorRitter, Jeremy S.en_US
dc.contributor.utaustinauthorSafranek-Shrader, Chalenceen_US
dc.contributor.utaustinauthorMilosavljevic, Milosen_US
dc.contributor.utaustinauthorBromm, Volkeren_US
dc.relation.ispartofserialAstrophysical Journalen_US


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