Fueling starburst galaxies with gas-rich mergers

Barnes, Joshua E.; Hernquist, Lars

doi:10.1086/185978

Cited by 940 publications

(976 citation statements)

References 0 publications

Supporting

Mentioning

911

Contrasting

Unclassified

Order By: Relevance

“…In this picture, gas is driven to the centre by tidal torques, where it is compressed and turns into stars at a very high rate (Barnes & Hernquist 1991). This was compatible with observations of ULIRGs which exhibit centrally concentrated star formation.…”

Section: Clumpy Star Formation Induced By Mergerssupporting

confidence: 85%

Enhancing and inhibiting star formation: high-resolution simulation studies of the impact of cold accretion, mergers and feedback on individual massive galaxies

Powell

Bournaud²,

Chapon³

et al. 2012

Proc. IAU

View full text Add to dashboard Cite

Abstract. The quest for a better understanding of the evolution of massive galaxies can be broadly summarised with 2 questions: how did they build up their large (stellar) masses and what eventually quenched their star formation (SF)? To tackle these questions, we use highresolution ramses simulations (Teyssier 2002) to study several aspects of the detailed interplay between accretion (mergers and cold flows), SF and feedback in individual galaxies. We examine SF in major mergers; a process crucial to stellar mass assembly. We explore whether the mergerinduced, clustered SF is as important a mechanism in average mergers, as it is in extreme systems like the Antennae. We find that interaction-induced turbulence drives up the velocity dispersion, and that there is a correlated rise in SFR in all our simulated mergers as the density pdf evolves to have an excess of very dense gas. Next, we introduce a new study into whether mechanical jet feedback can impact upon the ability of hot gas haloes to provide a supply of fuel for SF during mergers and in their remnants. Finally, we briefly review our recent study, in which we examine the effect of supernova (SN) feedback on galaxies accreting via the previously overlooked coldmode, by resimulating a stream-fed galaxy at z ∼ 9. A far-reaching galactic wind results yet it cannot suppress the cold, filamentary accretion or eject significant mass in order to reduce the SFR, suggesting that SN feedback may not be as effective as is often assumed.

show abstract

Section: Clumpy Star Formation Induced By Mergerssupporting

confidence: 85%

Enhancing and inhibiting star formation: high-resolution simulation studies of the impact of cold accretion, mergers and feedback on individual massive galaxies

Powell

Bournaud²,

Chapon³

et al. 2012

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…Work by several investigators confirms that tidal perturbations of gas-rich disk galaxies result in rapid gas inflows (Icke 1985, Noguchi 1988, Hernquist 1989, Barnes & Hernquist 1991. The immediate physical cause of these rapid inflows is a systematic transfer of angular momentum from the gas to the disk stars; tidally perturbed disks develop bars (or other non-axisymmetric structures) which exert gravitational torques on the gas (Combes, Dupraz, & Gerin 1990, Barnes & Hernquist 1991.…”

Section: Dissipation and Thermodynamicsmentioning

confidence: 96%

“…The immediate physical cause of these rapid inflows is a systematic transfer of angular momentum from the gas to the disk stars; tidally perturbed disks develop bars (or other non-axisymmetric structures) which exert gravitational torques on the gas (Combes, Dupraz, & Gerin 1990, Barnes & Hernquist 1991. Such inflows require strong shocks and rapid cooling, which work together to drive the gas irreversibly toward the center of the potential.…”

Section: Dissipation and Thermodynamicsmentioning

confidence: 99%

Dynamics of Galaxy Interactions

Barnes

1998

Saas-Fee Advanced Courses

Self Cite

View full text Add to dashboard Cite

Abstract. Interacting galaxies are a natural arena for studies of nonequilibrium stellar dynamics, gas dynamics, and thermodynamics. Only galaxy formation itself is as deeply concerned with as many different aspects of dynamics, and the connection between interactions and the formation of galaxies is probably no coincidence. This review discusses tidal interactions, halos and orbit decay, dissipative effects in galaxy interactions, properties of merger remnants, and origins of starbursts.

show abstract

“…We note that in barred and spiral galaxies the process of dissipation may determine the shape and location of the shocks as well as the gas in ow rate (Roberts, Shu & van Albada 1979, Barnes & Hernquist 1991. Whereas galactic disks are rather ine cient accretion disks (Steiman-Cameron & Durisen 1988) when shocks are formed in a non-axisymmetric gravitational potential mass transfer can occur rapidly (e. g. Mihos & Hernquist 1994a,b, Shlosman & Noguchi 1993.…”

Section: Summary and Discussionmentioning

confidence: 87%

Phase transitions in the ISM a source of dissipative behaviour

Quillen

1995

Astrophys Space Sci

View full text Add to dashboard Cite

In this paper, by considering a simple uid model, we investigate the role of phase transitions in the ISM on the galaxy scale gas dynamics. Cooling and heating timescales in the ISM are typically shorter than typical galactic rotation timescales, so the individual phases in the ISM can be assumed to be in temperature equilibrium with the radiation eld. Using this approximation we can construct an equation of state which depends upon the average density and mass fractions in the individual phases. Previous studies suggest that there is an equilibrium phase fraction as a function of pressure. We incorporate evolution towards this equilibrium state as a relaxation term with a time to obtain equilibrium . We derive a condition in terms of a critical Mach number when one dimensional shocks should be continuous. For small values of the relaxation time we show that the relaxation term acts like a viscosity. We show with one dimensional simulations that increasing causes shocks to become smoother. This work suggests that phase changes can strongly e ect the gas dynamics of the ISM across spiral arms and bars.

show abstract

Fueling starburst galaxies with gas-rich mergers

Cited by 940 publications

References 0 publications

Enhancing and inhibiting star formation: high-resolution simulation studies of the impact of cold accretion, mergers and feedback on individual massive galaxies

Enhancing and inhibiting star formation: high-resolution simulation studies of the impact of cold accretion, mergers and feedback on individual massive galaxies

Dynamics of Galaxy Interactions

Phase transitions in the ISM a source of dissipative behaviour

Contact Info

Product

Resources

About