3D simulations of clump formation in stellar wind collisions

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dc.catalogadorgjm
dc.contributor.authorCalderón Espinoza, Diego Nicolás
dc.contributor.authorCuadra, Jorge
dc.contributor.authorSchartmann, Marc
dc.contributor.authorBurkert, Andreas
dc.contributor.authorPrieto Brito, Joaquín
dc.contributor.authorRussell, Christopher M. P.
dc.date.accessioned2025-02-28T19:27:45Z
dc.date.available2025-02-28T19:27:45Z
dc.date.issued2019
dc.description.abstractThe inner parsec of our Galaxy contains tens of Wolf-Rayet stars whose powerful outflows are constantly interacting while filling the region with hot, diffuse plasma. Theoretical models have shown that, in some cases, the collision of stellar winds can generate cold, dense material in the form of clumps. However, their formation process and properties are not well understood yet. In this work we present, for the first time, a statistical study of the clump formation process in unstable wind collisions. We study systems with dense outflows (∼10−5 M yr−1 ), wind speeds of 500–1500 km s−1, and stellar separations of ∼20–200 au. We develop 3D high resolution hydrodynamical simulations of stellar wind collisions with the adaptive-mesh refinement grid-based code RAMSES. We aim to characterise the initial properties of clumps that form through hydrodynamic instabilities, mostly via the non-linear thin shell instability (NTSI). Our results confirm that more massive clumps are formed in systems whose winds are close to the transition between the radiative and adiabatic regimes. Increasing either the wind speed or the degree of asymmetry increases the dispersion of the clump mass and ejection speed distributions. Nevertheless, the most massive clumps are very light (∼10−3–10−2 M⊕), about three orders of magnitude less massive than theoretical upper limits. Applying these results to the Galactic Centre we find that clumps formed through the NTSI should not be heavy enough either to affect the thermodynamic state of the region or to survive for long enough to fall onto the central super-massive black hole.
dc.fechaingreso.objetodigital2025-02-28
dc.format.extent21 páginas
dc.fuente.origenRepositorio UC
dc.identifier.doi10.48550/arXiv.1906.04181
dc.identifier.urihttps://doi.org/10.48550/arXiv.1906.04181
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/102300
dc.identifier.wosidWOS:000518156100031
dc.information.autorucInstituto de Astrofísica; Calderón Espinoza, Diego Nicolás; 0000-0002-9019-9951; 224673
dc.information.autorucInstituto de Astrofísica; Cuadra, Jorge; S/I; 3855
dc.language.isoen
dc.nota.accesocontenido completo
dc.revistaArXiv e-prints
dc.rightsacceso abierto
dc.subjectHydrodynamics
dc.subjectInstabilities
dc.subjectGalaxy: centre
dc.subjectShock waves
dc.subjectStars: winds
dc.subjectOutflows
dc.subject.ddc520
dc.subject.deweyAstronomía
dc.title3D simulations of clump formation in stellar wind collisions
dc.typepreprint
sipa.codpersvinculados224673
sipa.codpersvinculados3855
sipa.trazabilidadORCID;20-04-2020
sipa.trazabilidadRepositorio UC;08-07-2021
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