Bar-Halo Interaction and Bar Growth

By E. Athanassoula. 2002

239 citations recorded by the source corpus.

I show that strong bars can grow in galactic disks, even when the latter are immersed in halos whose mass within the disk radius is comparable to, or larger than, the mass of the disk. I argue that this is due to the response of the halo and in particular to the destabilizing influence of the halo resonant stars. Via this instability mechanism, the halo can stimulate, rather than restrain, the growth of the bar.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ea8a77d77f843b162773da9cb2ce29d0a9a5b883

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. M. Cappellari
4. Thomas J. Cox
5. T. Naab
6. Volker Springel
7. R. Somerville
8. A. Dekel

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. M. Cappellari
4. Thomas J. Cox
5. J. Kormendy
6. T. Naab
7. R. Somerville
8. S. Khochfar

Citations in the corpus

• ARGOS – IV. The kinematics of the Milky Way bulge (2013, unknown): “(2006), and in numerical simulations (Athanassoula 2002).”
• Image decomposition of barred galaxies and AGN hosts (2007, result): “Athanassoula (2002, 2003) presents theoretical work which shows that bars get longer with age by capturing disc stars, which is in agreement with the observational findings in Gadotti & de Souza (2005) and GdS06, although more observational evidences are needed to settle this point.”
• On the nature of bulges in general and of box/peanut bulges in particular: input from N-body simulations (2005, background): “C© 2005 RAS nloaded from https://academ ic.oup.com /m nras/article/358/4/1477/1071570 by C N R S - ISTO user on 02 February 2021 N-body simulations have repeatedly shown that bars seen side-on1 have a boxy/peanut shape (e.g. Combes & Sanders 1981; Combes et al. 1990, hereafter CDFP90; Raha et al. 19”
• Generating Equilibrium Dark Matter Halos: Inadequacies of the Local Maxwellian Approximation (2003, background): “…& Goodman 1986; Velázquez & White 1999; Taylor & Babul 2001; Font et al. 2001), the susceptibility of disks to bar instabilities (Mihos, McGaugh, & de Blok 1997), and the effects of these bars on halo central density cusps (Debattista & Sellwood 2000; Athanassoula 2002; Valenzuela & Klypin 2003).”
• Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, methodology): “The effect of the halo relative mass on bar evolution is dual, as first discussed by Athanassoula (2002).”
• Simulating observations of dark matter dominated galaxies: towards the optimal halo profile (2002, background): “As bars are disk dynamical features (e.g., Athanassoula 2002), they imply a significant disk mass.”
• Galaxy Masses: A Review (2013, methodology): “1985; Sofue & Rubin 2001) but it is not by itself proof of dark matter in galaxies (see the prophetic contribution by Kalnajs in the 1982 Besancon conference proceedings Athanassoula (1983)). Despite notable efforts by the likes of Kapteyn, Oort, Babcock, Mayall, de Vaucouleurs, Schwarzschild, the B”
• Secular bar formation in galaxies with a significant amount of dark matter (2002, background): “Orbital resonances are blamed for the growth of bars (Athanassoula 2002).”
• Characterizing Bars at z ~ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift (2006, background): “…the angular momentum of the baryonic and dark matter components of disk galaxies (e.g., Weinberg 1985; Debattista & Sellwood 1998, 2000; Athanassoula 2002; Berentzen et al. 2006), thereby driving their dynamical and secular evolution (Kormendy 1993; for a review, see Kormendy &…”
• Properties of Bars and Bulges in the Hubble Sequence (2007, background): “…called buckling instability (Combes et al. 1990; Pfenniger & Friedli 1991; Raha et al. 1991; Berenzen et al. 1998; Athanassoula & Misioritis 2002; Athanassoula 2002, 2003, 2005a,b; O’Neilss & Dubinski 2003; Debattista et al. 2004; Martinez-Valpuesta, Shlosman & Heller 2004; Debattista et al.…”
• Multicomponent decompositions for a sample of S0 galaxies (2005, background): “…this paradox is resolved if it is assumed that there is angular momentum exchange between the bar and the spheroidal component: it was shown by Athanassoula (2002, 2003) that in the presence of a massive halo or a large massive bulge, angular momentum is emitted in the inner disc resonances…”
• Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution (2016, background): “(iii) The bar tends to be 3-5 disk scale-lengths long as already noted by Debattista & Sellwood (2000) and Athanassoula (2002).”
• The lifetime of galactic bars: central mass concentrations and gravity torques (2005, background): “In the two simulations with parameters typical of Sb-Sc galaxies, the cycle of bar dissolution takes about 2 Gyrs (for the mass and radius of the Milky-Way).”
• Bar Diagnostics in Edge-On Spiral Galaxies. III. N-Body Simulations of Disks (2004, methodology): “Athanassoula & Misiriotis (2002) and Athanassoula (2002, 2003a) also clearly showed that, even for highly concentrated and/or dominant halos, luminous matter can dominate the inner parts of the models at late times.”
• What determines the strength and the slowdown rate of bars (2003, background): “Several other ways have been put forward for the case of barred galaxies (Athanassoula 2002b) and they will be discussed in some detail in a future paper.”
• HOW DO DISKS SURVIVE MERGERS? (2008, background): “…it is well known from studies of isolated barred galaxies (e.g. Weinberg 1985; Hernquist & Weinberg 1992b; Friedli & Benz 1993; Friedli et al. 1994; Athanassoula 2002a; Athanassoula & Misiriotis 2002; Weinberg & Katz 2007; Kaufmann et al. 2007; Foyle et al. 2008) that a long-lived bar (regardless…”
• Galaxy formation theory (2010, background): “…evolution of bars, the importance of the dark matter halo and the cosmological evolution of the disk) remain poorly understood, but actively studied (Friedli and Benz 1993; Shlosman and Noguchi1993; El-Zant and Shlosman 2002; Athanassoula 2002; Bournaud and Combes 2002; Shen and Sellwood 2004).”
• BULGE n AND B/T IN HIGH-MASS GALAXIES: CONSTRAINTS ON THE ORIGIN OF BULGES IN HIERARCHICAL MODELS (2008, background): “Bars provide the most important internal mechanism for redistributing angular momentum in baryonic and dark matter components (e.g. Weinberg 1985; Debattista & Sellwood 1998, 2000; Athanassoula 2002; Berentzen, Shlosman, & Jogee 2006).”