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dc.contributor.authorLombardi, James C. Jr
dc.contributor.authorMcInally, William G.
dc.contributor.authorFaber, Joshua A.
dc.date.accessioned2015-06-19T15:49:09Z
dc.date.available2015-06-19T15:49:09Z
dc.date.issued2015-02-11
dc.identifier.citationLombardi, James C., Jr., William G. McInally, and Joshua A. Faber. 2015. "An efficient radiative cooling approximation for use in hydrodynamic simulations." Monthly Notices of the Royal Astronomical Society 447, no. 1: 25-35.en_US
dc.identifier.issn0035-8711
dc.identifier.issn1365-2966
dc.identifier.urihttp://hdl.handle.net/10456/38049
dc.description.abstractTo make relevant predictions about observable emission, hydrodynamical simulation codes must employ schemes that account for radiative losses, but the large dimensionality of accurate radiative transfer schemes is often prohibitive. Stamatellos and collaborators introduced a scheme for smoothed particle hydrodynamics (SPH) simulations based on the notion of polytropic pseudo-clouds that uses only local quantities to estimate cooling rates. The computational approach is extremely efficient and works well in cases close to spherical symmetry, such as in star formation problems. Unfortunately, the method, which takes the local gravitational potential as an input, can be inaccurate when applied to non-spherical configurations, limiting its usefulness when studying discs or stellar collisions, among other situations of interest. Here, we introduce the ‘pressure scale height method,’ which incorporates the fluid pressure scaleheight into the determination of column densities and cooling rates, and show that it produces more accurate results across a wide range of physical scenarios while retaining the computational efficiency of the original method. The tested models include spherical polytropes as well as discs with specified density and temperature profiles. We focus on applying our techniques within an SPH code, although our method can be implemented within any particle-based Lagrangian or grid-based Eulerian hydrodynamic scheme. Our new method may be applied in a broad range of situations, including within the realm of stellar interactions, collisions, and mergers.en_US
dc.language.isoen_USen_US
dc.publisherOxford University Pressen_US
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen_US
dc.relation.isversionofhttp://dx.doi.org/10.1093/mnras/stu2432en_US
dc.rightsThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.en_US
dc.subjecthydrodynamicsen_US
dc.subjectradiative transferen_US
dc.subjectmethods: numericalen_US
dc.subjectprotoplanetary discsen_US
dc.subjectcircumstellar matteren_US
dc.subjectstars: formationen_US
dc.titleAn efficient radiative cooling approximation for use in hydrodynamic simulationsen_US
dc.description.versionPublished articleen_US
dc.contributor.departmentPhysicsen_US
dc.citation.volume447en_US
dc.citation.issue1en_US
dc.citation.spage25en_US
dc.citation.epage35en_US
dc.identifier.doi10.1093/mnras/stu2432
dc.contributor.avlauthorLombardi, James C. Jr


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