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dc.contributor.authorSchneider, Evan E.
dc.contributor.authorRobertson, Brant E.
dc.date.accessioned2017-04-11T19:02:03Z
dc.date.available2017-04-11T19:02:03Z
dc.date.issued2017-01-10
dc.identifier.citationHYDRODYNAMICAL COUPLING OF MASS AND MOMENTUM IN MULTIPHASE GALACTIC WINDS 2017, 834 (2):144 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/834/2/144
dc.identifier.urihttp://hdl.handle.net/10150/623100
dc.description.abstractUsing a set of high-resolution hydrodynamical simulations run with the Cholla. code, we investigate how mass and momentum couple to the multiphase components of galactic winds. The simulations model the interaction between a hot wind driven by supernova explosions and a cooler, denser cloud of interstellar or circumgalactic media. By resolving scales of Delta x < 0.1 pc over > 100 pc distances, our calculations capture how the cloud disruption leads to a distribution of densities and temperatures in the resulting multiphase outflow and quantify the mass and momentum associated with each phase. We find that the multiphase wind contains comparable mass and momenta in phases over a wide range of densities and temperatures extending from the hot wind (n approximate to 10(-2.5) cm(-3), T approximate to 10(6.5) K) to the coldest components (n approximate to 10(2) cm(-3), T approximate to 10(2) K). We further find that the momentum distributes roughly in proportion to the mass in each phase, and the mass loading of the hot phase by the destruction of cold, dense material is an efficient process. These results provide new insight into the physical origin of observed multiphase galactic outflows and inform galaxy formation models that include coarser treatments of galactic winds. Our results confirm that cool gas observed in outflows at large distances from the galaxy (greater than or similar to 1 kpc) likely does not originate through the entrainment of cold material near the central starburst.
dc.description.sponsorshipNational Science Foundation [1228509]; DOE Office of Science User Facility [DE-AC05-00OR22725]en
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/834/i=2/a=144?key=crossref.e25f767345ce4ccf39509c9438a0088cen
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.subjectgalaxies: evolutionen
dc.subjecthydrodynamicsen
dc.subjectISM: cloudsen
dc.subjectsupernovae: generalen
dc.subjectturbulenceen
dc.titleHYDRODYNAMICAL COUPLING OF MASS AND MOMENTUM IN MULTIPHASE GALACTIC WINDSen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-11T18:31:14Z
html.description.abstractUsing a set of high-resolution hydrodynamical simulations run with the Cholla. code, we investigate how mass and momentum couple to the multiphase components of galactic winds. The simulations model the interaction between a hot wind driven by supernova explosions and a cooler, denser cloud of interstellar or circumgalactic media. By resolving scales of Delta x < 0.1 pc over > 100 pc distances, our calculations capture how the cloud disruption leads to a distribution of densities and temperatures in the resulting multiphase outflow and quantify the mass and momentum associated with each phase. We find that the multiphase wind contains comparable mass and momenta in phases over a wide range of densities and temperatures extending from the hot wind (n approximate to 10(-2.5) cm(-3), T approximate to 10(6.5) K) to the coldest components (n approximate to 10(2) cm(-3), T approximate to 10(2) K). We further find that the momentum distributes roughly in proportion to the mass in each phase, and the mass loading of the hot phase by the destruction of cold, dense material is an efficient process. These results provide new insight into the physical origin of observed multiphase galactic outflows and inform galaxy formation models that include coarser treatments of galactic winds. Our results confirm that cool gas observed in outflows at large distances from the galaxy (greater than or similar to 1 kpc) likely does not originate through the entrainment of cold material near the central starburst.


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