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Tracing the evolution of radiation-MHD simulations of solar and stellar atmospheres in the Lagrangian frame
Stockholm University, Faculty of Science, Department of Astronomy.
Number of Authors: 12018 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 616, article id A136Article in journal (Refereed) Published
Abstract [en]

Context. Radiation magnetohydrodynamics (radiation-MHD) simulations have become a standard tool for investigating the physics of solar and stellar atmospheres. Aims. The aim of this paper is to present a method that allows the efficient and accurate analysis of flows in such simulations in the Lagrangian frame. Methods. This paper presents a method that allows the construction of pathlines given a seed point that can be chosen freely at any location and at any time during the simulation where the simulation state is stored. The method is based on passive tracer particles. Through injection of particles in expanding regions the occurrence of particle-free volumes is avoided, even in the case of strongly compressive flows. Results. The method was implemented in the solar and stellar atmosphere simulation code Bifrost. It is efficient and accurate. As examples I present an analysis of a gas parcel in the convection zone and a particle in the solar transition region.

Place, publisher, year, edition, pages
2018. Vol. 616, article id A136
Keywords [en]
Sun: atmosphere, methods: numerical
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-160062DOI: 10.1051/0004-6361/201833176ISI: 000443099000001OAI: oai:DiVA.org:su-160062DiVA, id: diva2:1254451
Available from: 2018-10-09 Created: 2018-10-09 Last updated: 2018-10-09Bibliographically approved

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Leenaarts, Jorrit
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