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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7473
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dc.contributor.authorVijayan, Aditi-
dc.contributor.authorKim, Chang-Goo-
dc.contributor.authorArmillotta, Lucia-
dc.contributor.authorOstriker, Eve C-
dc.contributor.authorLi, Miao-
dc.date.accessioned2020-05-27T06:56:51Z-
dc.date.available2020-05-27T06:56:51Z-
dc.date.issued2020-05-
dc.identifier.citationThe Astrophysical Journal, 2020, Vol.894, Article No.12en_US
dc.identifier.issn0004-637X-
dc.identifier.issn1538-4357(Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7473-
dc.descriptionOpen Accessen_US
dc.description.abstractGalactic outflows produced by stellar feedback are known to be multiphase in nature. Observations and simulations indicate that the material within several kiloparsecs of galactic disk midplanes consists of warm clouds embedded within a hot wind. A theoretical understanding of the outflow phenomenon, including both winds and fountain flows, requires study of the interactions among thermal phases. We develop a method to quantify these interactions via measurements of mass, momentum, and energy flux exchanges using temporally and spatially averaged quantities and conservation laws. We apply this method to a star-forming interstellar medium simulation based on the TIGRESS framework, for solar neighborhood conditions. To evaluate the extent of interactions among the phases, we examine the validity of the "ballistic model," which predicts the trajectories of the warm phase (5050 K < T < 2 × 104 K) treated as non-interacting clouds. This model is successful at intermediate vertical velocities ( 50kms−1≲|vz|≲100kms−1 ), but at higher velocities, we observe an excess in simulated warm outflow compared to the ballistic model. This discrepancy cannot be fully accounted for by cooling of high-velocity, intermediate-temperature (2 × 104 K < T < 5 × 105 K) gas. We examine the fluxes of mass, momentum, and energy and conclude that the warm phase gains mass via cooling of the intermediate phase and momentum from the hot (T > 5 × 105 K) phase. The large energy flux from the hot outflow, transferred to the warm and intermediate phases, is quickly radiated away. A simple interaction model implies an effective warm cloud size in the fountain flow of a few 100 pc, showing that warm-hot flux exchange mainly involves a few large clouds rather than many small ones.en_US
dc.language.isoenen_US
dc.publisherIOP Sciences for The American Astronomical Societyen_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2020ApJ...894...12V/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1911.07872en_US
dc.relation.urihttps://doi.org/10.3847/1538-4357/ab8474en_US
dc.rights2020, The American Astronomical Societyen_US
dc.subjectMagnetohydrodynamical simulationsen_US
dc.subjectInterstellar mediumen_US
dc.subjectGalaxy fountainsen_US
dc.subjectGalaxy windsen_US
dc.subjectStellar feedbacken_US
dc.titleKinematics and Dynamics of Multiphase Outflows in Simulations of the Star-forming Galactic Interstellar Mediumen_US
dc.typeArticleen_US
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