Multi-Dimensional Simulations Of Rotating Pair-Instability Supernovae

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dc.contributor.utaustinauthorChatzopoulos, Emmanouilen_US
dc.contributor.utaustinauthorWheeler, J. Craigen_US
dc.creatorChatzopoulos, Emmanouilen_US
dc.creatorWheeler, J. Craigen_US
dc.creatorCouch, Sean M.en_US
dc.date.accessioned2016-04-28T19:35:11Z
dc.date.available2016-04-28T19:35:11Z
dc.date.issued2013-10en
dc.description.abstractWe study the effects of rotation on the dynamics, energetics, and Ni-56 production of pair instability supernova (PISN) explosions by performing rotating two-dimensional ("2.5D") hydrodynamics simulations. We calculate the evolution of eight low-metallicity (Z = 10(-3), 10(-4) Z(circle dot)) massive (135-245 M-circle dot) PISN progenitors with initial surface rotational velocities of 50% of the critical Keplerian value using the stellar evolution code MESA. We allow for both the inclusion and the omission of the effects of magnetic fields in the angular momentum transport and in chemical mixing, resulting in slowly rotating and rapidly rotating final carbon-oxygen cores, respectively. Increased rotation for carbon-oxygen cores of the same mass and chemical stratification leads to less energetic PISN explosions that produce smaller amounts of Ni-56 due to the effect of the angular momentum barrier that develops and slows the dynamical collapse. We find a non-monotonic dependence of Ni-56 production on rotational velocity in situations when smoother composition gradients form at the outer edge of the rotating cores. In these cases, the PISN energetics are determined by the competition of two factors: the extent of chemical mixing in the outer layers of the core due to the effects of rotation in the progenitor evolution and the development of angular momentum support against collapse. Our 2.5D PISN simulations with rotation are the first presented in the literature. They reveal hydrodynamic instabilities in several regions of the exploding star and increased explosion asymmetries with higher core rotational velocity.en_US
dc.description.departmentAstronomyen_US
dc.description.sponsorshipSTScI AR12820en_US
dc.description.sponsorshipUniversity of Texas Graduate School William C. Powers fellowshipen_US
dc.description.sponsorshipNSF PHY-1066293en_US
dc.identifierdoi:10.15781/T2KF8V
dc.identifier.Filename2013_10_multidimensional.pdfen_US
dc.identifier.citationChatzopoulos, Emmanouil, J. Craig Wheeler, and Sean M. Couch. "Multi-dimensional Simulations of Rotating Pair-instability Supernovae." The Astrophysical Journal, Vol. 776, No. 2 (Oct., 2013): 129.en_US
dc.identifier.doi10.1088/0004-637x/776/2/129en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/2152/34822
dc.language.isoEnglishen_US
dc.relation.ispartofen_US
dc.relation.ispartofserialAstrophysical Journalen_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.rights.restrictionOpenen_US
dc.subjectstars: evolutionen_US
dc.subjectstars: massiveen_US
dc.subjectstars: rotationen_US
dc.subjectsupernovae: generalen_US
dc.subjectsupernovae: individualen_US
dc.subjectpopulation iii protostarsen_US
dc.subjectstellar astrophysics mesaen_US
dc.subjectgamma-ray burstsen_US
dc.subjectm-circle-doten_US
dc.subjectmassive starsen_US
dc.subject1st starsen_US
dc.subjectmagnetic-fieldsen_US
dc.subjectpresupernovaen_US
dc.subjectevolutionen_US
dc.subjectdifferential rotationen_US
dc.subjectluminous supernovaeen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleMulti-Dimensional Simulations Of Rotating Pair-Instability Supernovaeen_US
dc.typeArticleen_US

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