Evolution of Stellar Bars in Live Axisymmetric Halos: Recurrent Buckling and Secular Growth
By I. Martinez-Valpuesta, I. Shlosman, C. Heller. 2005
304 citations recorded by the source corpus.
Evolution of stellar bars in disk galaxies is accompanied by dynamical instabilities and secular changes. Following the vertical buckling instability, the bars are known to weaken dramatically and develop a pronounced boxy/peanut shape when observed edge-on. Using high-resolution N-body simulations of stellar disks embedded in live axisymmetric dark matter halos, we have investigated the long-term changes in the bar morphology, specifically the evolution of the bar size, its vertical structure, and the exchange of angular momentum. We find that following the initial buckling, the bar resumes its growth from deep inside the corotation radius and follows the ultraharmonic resonance thereafter. We also find that this secular bar growth triggers a spectacular secondary vertical buckling instability that leads to the appearance of characteristic boxy/peanut/X-shaped bulges. The secular bar growth is crucial for the recurrent buckling to develop. Furthermore, the secondary buckling is milder, persists over a substantial period of time, ~3 Gyr, and can have observational counterparts. Overall, the stellar bars show recurrent behavior in their properties and evolve by increasing their linear and vertical extents, both dynamically and secularly. We also demonstrate explicitly that the prolonged growth of the bar is mediated by continuous angular momentum transfer from the disk to the surrounding halo and that this angular momentum redistribution is resonant in nature: a large number of lower resonances trap disk and halo particles, and this trapping is robust, in broad agreement with the earlier results in the literature.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/3be351eec8b8fc5ddb916a17176534fc4e871412
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Citations in the corpus
- Reddening and metallicity maps of the Milky Way bulge from VVV and 2MASS II. The complete high resolution extinction map and implications for Galactic bulge studies (2012, methodology): “With our full extinction map, it is possible to compare the global GB structure to models such as that of Martinez-Valpuesta et al. (2006).”
- The structure of the Milky Way's bar outside the bulge (2015, background): “This is similar to the structures found in N-body simulations where the buckled three-dimensional boxy/peanut bulge is shorter than the bar (e.g. Athanassoula 2005; Martinez-Valpuesta et al. 2006), as well as in external galaxies (Erwin & Debattista 2013).”
- The Secular Evolution of Disk Structural Parameters (2005, background): “After this bend has dissipated, the process repeats another two times (see also Martinez-Valpuesta et al. 2006), with small bends on the leading side of the bar, developing into stronger bends on crossing the bar’s major axis.”
- Mapping the three-dimensional density of the galactic bulge with VVV red clump stars (2013, background): “The resultant three dimensional density of the bulge prominently displays a boxy/peanut-like structure, qualitatively very similar to that predicted by N-body simulations of the buckling instability (e.g. Athanassoula & Misiriotis 2002; Martinez-Valpuesta et al. 2006).”
- Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution (2016, methodology): “During the evolution the disk becomes unstable and forms a bar, that later forms a B/P bulge thought the buckling instability mechanism (Combes et al. 1990; Martinez-Valpuesta et al. 2006).”
- The population of barred galaxies in the local universe - I. Detection and characterisation of bars (2009, background): “…rotations because of large-scale violent bending instabilities and settle with an increased thickness and vertical velocity dispersion (e.g., Combes & Sanders 1981; Combes et al. 1990; Raha et al. 1991; Athanassoula 2003; Debattista et al. 2004; Athanassoula 2005; Martinez-Valpuesta et al. 2006).”
- Characterizing Bars at z ~ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift (2006, methodology): “…2003), the central mass concentrations (CMCs) present in the inner few hundred parsecs (e.g., Shen & Sellwood 2004; Athanassoula et al. 2005;Martinez-Valpuesta et al. 2006; Debattista et al. 2006), and the distribution and amount of gas in the disk (e.g., Shlosman & Noguchi 1993; Bournaud…”
- Bars in Disk-dominated and Bulge-dominated Galaxies at z ~ 0: New Insights from ~3600 SDSS Galaxies (2007, background): “Most simulations (Shen & Sellwood 2004; Athanassoula et al. 2005; Martinez-Valpuesta et al. 2006; Debattista et al. 2006) indicate that present-day bars are relatively robust against the type of central mass concentrations (CMCs) and B/D that exist in present-day galaxies today or in the recent…”
- BULGE n AND B/T IN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS (2008, background): “Boxy/peanut bulges are believed to be the result of vertical resonances and buckling instabilities in bars, which are viewed at high inclination (Combes & Sanders 1981; Combes et al. 1990; Pfenniger & Norman 1990; Bureau & Athanassoula 2005; Athanassoula 2005; Martinez-Valpuesta et al. 2006).”
- The Galaxy and its stellar halo: insights on their formation from a hybrid cosmological approach (2008, background): “…of disk instability is very simplified, and gives a very crude description of the complex phenomenology associated to bar formation and evolution, which is the subject of current active research (Martinez-Valpuesta et al. 2006; Berentzen et al. 2007; Curir et al. 2007, and references therein).”