Gas accretion on spiral galaxies: Bar formation and renewal

By Frédéric Bournaud, F. C. E. N. Superieure, París, France., Lerma, O. Paris. 2002

263 citations recorded by the source corpus.

The eects of gas accretion on spiral disk dynamics and stability are studied through N-body simulations, including star formation and gas/stars mass exchange. The detailed processes of bar formation, bar destruction and bar re-formation are followed, while in the same time the disk to bulge ratio is varying. The accreted gas might be first prevented to flow inwards to the center by the bar gravity torques, which maintains it to the outer Lindblad resonance. While the first bar is weakening, the accreted gas replenishes the disk, increasing the disk-to-bulge ratio, and the disk self-gravity. A second bar is then unstable, with a higher pattern speed, due both to the increased mass, and shorter bar length. Three or four bar episodes have been followed over a Hubble time. Their strength is decreasing with time, while their pattern speed is increasing. Detailed balance of the angular momentum transfer and evolution can account for these processes. The gas recycled through star formation, and rejected through stellar mass loss plays also a role in the disk dynamics. Implications on the spiral galaxy dynamics and evolution along the Hubble sequence, and as a function of redshift are discussed.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/38c13c27bf5d8f40de133789b7a7736d021283a2

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. A. Dekel
4. R. Dav'e
5. T. Naab
6. E. Quataert
7. R. Somerville
8. Thomas J. Cox

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. A. Dekel
4. Frédéric Bournaud
5. Thomas J. Cox
6. E. Quataert
7. T. Naab
8. R. Dav'e

Citations in the corpus

• A NEW MECHANISM FOR RADIAL MIGRATION IN GALACTIC DISKS: SPIRAL–BAR RESONANCE OVERLAP (2009, background): “…MW bar and SS, but it is reasonable to expect more realistic scenarios, where throughout the lifetime of the Galaxy there could have been variations of the perturbers’ amplitudes and pattern speeds, bar size, spiral pitch angle, as well as bar destruction and reformation (Bournaud and Combes 2002).”
• Rapid Formation of Exponential Disks and Bulges at High Redshift from the Dynamical Evolution of Clump-Cluster and Chain Galaxies (2007, methodology): “Code description We model the evolution of Jeans-unstable gas-rich galactic disks using a particle-mesh sticky-particle code (see Bournaud & Combes 2002, 2003).”
• Secular Evolution via Bar-driven Gas Inflow: Results from BIMA SONG (2005, background): “…sequence could be the dissolution of bars by an increasing central concentration of mass. Models have debated the exact impact of increasing central concentration (e.g., Friedli & Benz 1993; Norman, Sellwood, & Hasan 1996; Bournaud & Combes 2002; Athanassoula 2003; Shen & Sellwood 2004).”
• Evolution of galactic discs: multiple patterns, radial migration, and disc outskirts (2012, background): “The gSb bar is weaker because the gas fraction is higher, and when the gas is driven to the center by the bar, it actually weakensthe bar (Bournaud and Combes, 2002; Bournaud et al., 2005).”
• How do massive black holes get their gas (2009, background): “…which is applicable to the intermediate scales (∼10–100 pc) in our simulations (see e.g. Bardeen 1975; Narayan, Goldreich & Goodman 1987; Raha et al. 1991; Christodoulou, Shlosman & Tohline 1995; Earn & Sellwood 1995; Bournaud & Combes 2002; Athanassoula 2008; Dubinski, Berentzen & Shlosman 2009).”
• Bar Diagnostics in Edge-On Spiral Galaxies. III. N-Body Simulations of Disks (2004, background): “Total bar disruption (e.g., Pfenniger & Norman 1990; Friedli & Benz 1993) is also in conflict with the large fraction of bars observed, unless they can be regenerated rapidly, which requires substantial external gas accretion (e.g., Bournaud & Combes 2002).”
• Evidence for strong dynamical evolution in disc galaxies through the last 11 Gyr. GHASP VIII – a local reference sample of rotating disc galaxies for high‐redshift studies (2009, background): “…flows (Dekel et al. 2009; Kereš et al. 2009) and other types of diffuse gas accretion (Semelin & Combes 2005), bulges form by internal and clump-driven evolution (Elmegreen et al. 2008; Genzel et al. 2008), and the thin disk forms later by further smooth accretion (e.g., Bournaud & Combes 2002).”
• Molecular gas in NUclei of GAlaxies (NUGA) - IV. Gravitational torques and AGN feeding (2005, unknown): “When there are several stellar pattern speeds at different radii in a galaxy disk, numerical simulations show that the gas response tends to be coupled with the stellar potential pattern (Friedli & Benz 1995; García-Burillo et al. 1998; Bournaud & Combes 2002, 2005, in prep.).”
• On the nature of bulges in general and of box/peanut bulges in particular: input from N-body simulations (2005, background): “…of the necessary mass and of its central concentration (Hasan, Pfenniger & Norman 1993; Friedli 1994; Norman, Sellwood & Hasan 1996; Hozumi & Hernquist 1998, 1999; Berentzen et al. 1998; Bournaud & Combes 2002; Shen & Sellwood 2004; Athanassoula, Dehnen & Lambert 2005, and in preparation).”
• Chemodynamical evolution of the Milky Way disk - I. The solar vicinity (2012, background): “It may also give rise to a more unstable disk, while suppressing the bar instability (e.g., Bournaud and Combes 2002).”
• CONSTRAINTS ON THE ASSEMBLY AND DYNAMICS OF GALAXIES. II. PROPERTIES OF KILOPARSEC-SCALE CLUMPS IN REST-FRAME OPTICAL EMISSION OF z ∼ 2 STAR-FORMING GALAXIES (2011, background): “…1999; Immeli et al. 2004a,b; Bournaud et al. 2007; Carollo et al. 2007; Elmegreen et al. 2009a; Ceverino et al. 2010), along with other internal mechanisms such as stellar bar-induced streaming (e.g., Bournaud & Combes 2002) or viscous drag in a gaseous disk (e.g., Lin & Pringle 1987; Silk 2001).”
• The population of barred galaxies in the local universe - I. Detection and characterisation of bars (2009, background): “Some numerical simulations of bar formation and evolution propose that bars can be formed and destroyed fastly due to the accretion of gas towards the central regions of the galaxies (Pfenniger & Norman 1990; Bournaud & Combes 2002; Bournaud et al. 2005).”
• MORPHOLOGICAL QUENCHING OF STAR FORMATION: MAKING EARLY-TYPE GALAXIES RED (2009, methodology): “The code we use for the re-simulation is the Particle-Mesh code described in Bournaud & Combes (2002, 2003).”
• Nobeyama CO Atlas of Nearby Spiral Galaxies: Distribution of Molecular Gas in Barred and Nonbarred Spiral Galaxies (2007, background): “It is still an open question as to whether bars are short lived due to destruction by mass transport toward the center or not (e.g., Bournaud & Combes 2002; Das et al. 2003; Shen & Sellwood 2004; Bournaud et al. 2005; Athanassoula et al. 2005).”
• Bar formation and evolution in disc galaxies with gas and a triaxial halo: morphology, bar strength and halo properties (2012, background): “A number of studies including gas have given important insight (e.g. Berentzen et al. 1998, 2003, 2004, 2007; Bournaud & Combes 2002; Bournaud, Combes & Semelin 2005; Debattista et al. 2006; Heller, Shlosman & Athanassoula 2007a,b; Wozniak & Michel-Dansac 2009; Villa-Vargas, Shlosman & Heller 2010;…”
• From Rings to Bulges: Evidence for Rapid Secular Galaxy Evolution at z ~ 2 from Integral Field Spectroscopy in the SINS Survey (2008, background): “Other secular processes in a stellar disk, such as bar formation and transport, occur on a timescale tbar 30Y50 tdyn(R6) ( Immeli et al. 2004a, 2004b; Bournaud & Combes 2002).”
• What drives the growth of black holes (2011, background): “…major mergers have the potential to remove significant amounts of angular momentum and drive the gas into the central regions of galaxies (e.g., Shlosman et al., 1989, 1990; Barnes & Hernquist, 1992, 1996; Mihos & Hernquist, 1996; Bournaud & Combes, 2002; Garcı́aBurillo et al., 2005); see Fig.”
• Dissecting simulated disc galaxies - I. The structure of mono-age populations (2014, methodology): “For that we use the Particle-Mesh code described in Bournaud & Combes (2002, 2003), with gas dynamics modelled by a sticky-particle algorithm.”
• Characterizing Bars at z ~ 0 in the Optical and NIR: Implications for the Evolution of Barred Disks with Redshift (2006, background): “…easy destruction occurs, then there must be a very efficient mechanism that not only regenerates bars on a short timescale (e.g., Block et al. 2002; Bournaud & Combes 2002) but is also very well tuned to the bar destruction rate so that it can reproduce the observed constant optical bar fraction…”
• Multiple minor mergers: formation of elliptical galaxies and constraints for the growth of spiral disks (2007, methodology): “The dissipative dynamics of the ISM has been accounted for by the sticky-particles scheme described in Appendix A of Bournaud & Combes (2002).”