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dc.contributor.authorFalceta-Gonçalves, D.
dc.contributor.authorMonteiro, H.
dc.identifier.citationFalceta-Gonçalves , D & Monteiro , H 2014 , ' On the alignment of PNe and local magnetic field at the Galactic centre : magnetohydrodynamical numerical simulations ' Monthly Notices of the Royal Astronomical Society , vol 438 , no. 4 , pp. 2853-2863 . DOI: 10.1093/mnras/stt2393en
dc.identifier.otherPURE: 146984388
dc.identifier.otherPURE UUID: 9879756e-2327-43c7-a2d2-b9534fc619c4
dc.identifier.otherScopus: 84894361217
dc.descriptionDFG thanks the European Research Council (ADG-2011 ECOGAL), and Brazilian agencies CNPq (no. 300382/2008-1), CAPES (3400-13-1) and FAPESP (no.2011/12909-8) for financial support. HM thanks CNPq grant 573648/2008-5 and FAPEMIG grants APQ-02030-10 and CEX-PPM-00235-12.en
dc.description.abstractFor the past decade, observations of the alignment of planetary nebulae (PNe) symmetries with respect to the Galactic disc have led to conflicting results. Recently, the first direct observational evidence for a real alignment between PNe and local interstellar magnetic fields in the central part of the Galaxy (b <5°) has been found. Motivated by the recent discovery, we studied the role of the interstellar magnetic field on the dynamical evolution of a planetary nebula by means of an analytical model and from 3D magnetohydrodynamical numerical simulations. In our models, the nebula is the result of a short-time event of mass ejection with its surrounding medium. The nebula asphericity is assumed to be due to an intrinsic shaping mechanism, dominated by the latitude-dependent asymptotic giant branch wind, and not the interstellar medium field. We test under what conditions typical ejecta would have their dynamics severely modified by an interstellar magnetic field. We found that uniform fields of > 100 μG are required in order to be dynamically dominant. This is found to occur only at later evolutionary stages, therefore, being unable to change the general morphology of the nebula. However, the symmetry axis of bipolar and elliptical nebulae end up aligned to the external field. This result can explain why different samples of PNe result in different conclusions regarding the alignment of PNe. Objects located at high Galactic latitudes, or at large radii, should present no preferential alignment with respect to the Galactic plane. PNe located at the Galactic centre and low latitudes would, on the other hand, be preferentially aligned to the disc. Finally, we present synthetic polarization maps of the nebulae to show that the polarization vectors, as well as the field lines at the expanding shell, are not uniform even in the strongly magnetized case, indicating that polarization maps of nebulae are not adequate in probing the orientation, or intensity, of the dominant external field.en
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Societyen
dc.subjectMethods: numericalen
dc.subjectISM: magnetic fieldsen
dc.subjectPlanetary nebulae: generalen
dc.subjectGalaxy: bulgeen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleOn the alignment of PNe and local magnetic field at the Galactic centre : magnetohydrodynamical numerical simulationsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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