GEPI, Observatoire de Paris, PSL Research University, Place Jules Janssen, F-92190 Meudon, France, LERMA, Observatoire de Paris, CNRS, PSL University, Sorbonne Universités, UPMC Univ. Paris 06, F-75014 Paris, France
Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany
Leibniz Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany, Institute of Astronomy, Russian Academy of Sciences, 48 Pyatnitskya St, Moscow 119017, Russia, Max Planck Institute for Extraterrestrial Physics, D-85741 Garching, Germany
GEPI, Observatoire de Paris, PSL Research University, Place Jules Janssen, F-92190 Meudon, France
LERMA, Observatoire de Paris, CNRS, PSL University, Sorbonne Universités, UPMC Univ. Paris 06, F-75014 Paris, France, Collège de France, 12 Place Marcelin-Berthelot, F-75005 Paris, France
Boxy, peanut-, or X-shaped ‘bulges’ are observed in a large fraction of barred galaxies viewed in, or close to, edge-on projection, as well as in the Milky Way. They are the product of dynamical instabilities occurring in stellar bars, which cause the latter to buckle and thicken vertically. Recent studies have found nearby galaxies that harbour two such features arising at different radial scales, in a nested configuration. In this paper, we explore the formation of such double peanuts, using a collisionless N-body simulation of a pure disc evolving in isolation within a live dark matter halo, which we analyse in a completely analogous way to observations of real galaxies. In the simulation, we find a stable double configuration consisting of two X/peanut structures associated with the same galactic bar – rotating with the same pattern speed – but with different morphology, formation time, and evolution. The inner, conventional peanut-shaped structure forms early via the buckling of the bar, and experiences little evolution once it stabilizes. This feature is consistent in terms of size, strength, and morphology, with peanut structures observed in nearby galaxies. The outer structure, however, displays a strong X, or ‘bow-tie’, morphology. It forms just after the inner peanut, and gradually extends in time (within 1–1.5 Gyr) to almost the end of the bar, a radial scale where ansae occur. We conclude that, although both structures form, and are dynamically coupled to, the same bar, they are supported by inherently different mechanisms.
Ciambur, Bogdan C., et al. "Double X/Peanut structures in barred galaxies – insights from an <i>N</i> -body simulation." Monthly Notices of the Royal Astronomical Society, vol. 503, no. 2, Dec. 2020. https://doi.org/10.1093/mnras/staa3814
Ciambur, Bogdan C., Fragkoudi, Francesca, Khoperskov, Sergey, et al., "Double X/Peanut structures in barred galaxies – insights from an <i>N</i> -body simulation," Monthly Notices of the Royal Astronomical Society 503, no. 2 (2020), https://doi.org/10.1093/mnras/staa3814
@article{osti_1772843,
author = {Ciambur, Bogdan C. and Fragkoudi, Francesca and Khoperskov, Sergey and Di Matteo, Paola and Combes, Françoise},
title = {Double X/Peanut structures in barred galaxies – insights from an <i>N</i> -body simulation},
annote = {ABSTRACT Boxy, peanut-, or X-shaped ‘bulges’ are observed in a large fraction of barred galaxies viewed in, or close to, edge-on projection, as well as in the Milky Way. They are the product of dynamical instabilities occurring in stellar bars, which cause the latter to buckle and thicken vertically. Recent studies have found nearby galaxies that harbour two such features arising at different radial scales, in a nested configuration. In this paper, we explore the formation of such double peanuts, using a collisionless N-body simulation of a pure disc evolving in isolation within a live dark matter halo, which we analyse in a completely analogous way to observations of real galaxies. In the simulation, we find a stable double configuration consisting of two X/peanut structures associated with the same galactic bar – rotating with the same pattern speed – but with different morphology, formation time, and evolution. The inner, conventional peanut-shaped structure forms early via the buckling of the bar, and experiences little evolution once it stabilizes. This feature is consistent in terms of size, strength, and morphology, with peanut structures observed in nearby galaxies. The outer structure, however, displays a strong X, or ‘bow-tie’, morphology. It forms just after the inner peanut, and gradually extends in time (within 1–1.5 Gyr) to almost the end of the bar, a radial scale where ansae occur. We conclude that, although both structures form, and are dynamically coupled to, the same bar, they are supported by inherently different mechanisms.},
doi = {10.1093/mnras/staa3814},
url = {https://www.osti.gov/biblio/1772843},
journal = {Monthly Notices of the Royal Astronomical Society},
issn = {ISSN 0035-8711},
number = {2},
volume = {503},
place = {United Kingdom},
publisher = {Oxford University Press},
year = {2020},
month = {12}}
Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 2 Vol. 503; ISSN 0035-8711
PLANETARY NEBULAE AS ASTRONOMICAL TOOLS: International Conference on Planetary Nebulae as Astronomical Tools, AIP Conference Proceedingshttps://doi.org/10.1063/1.2146306