Shock-induced star formation in a model of the Mice

By J. Barnes. 2004

149 citations recorded by the source corpus.

Star formation plays an important role in the fate of interacting galaxies. To date, most galactic simulations including star formation have used a density-dependent star formation rule designed to approximate a Schmidt law. Here, I present a new star formation rule which is governed by the local rate of energy dissipation in shocks. The new and old rules are compared using self-consistent simulations of NGC 4676; shock-induced star formation provides a better match to the observations of this system.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/6ebb41b618bdb2f0753779ee372fc9b1b04d8f86

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. Thomas J. Cox
4. R. Dav'e
5. R. Somerville
6. Volker Springel
7. A. Dekel
8. E. Quataert

In Instrumentation

1. P. Hopkins
2. L. Hernquist
3. Thomas J. Cox
4. R. Somerville
5. A. Dekel
6. R. Dav'e
7. E. Quataert
8. Volker Springel

Citations in the corpus

• Metallicity and Nuclear Star Formation in Nearby Galaxy Pairs: Evidence for Tidally Induced Gas Flows (2005, background): “Tidal interactions and associated shocks are thought to trigger star formation (e.g., Bushouse 1987; Kennicutt et al. 1987; Barnes 2004).”
• Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate (2005, background): “…the complexity of these processes, it has been impossible to converge on a robust description of star formation; instead, a wide range of empirically motivated prescriptions on kiloparsec or larger scales have been adopted (e.g., Somerville & Primack 1999; Springel & Hernquist 2003a; Barnes 2004).”
• Modelling feedback from stars and black holes in galaxy mergers (2004, background): “For example, Barnes (2004) has recently proposed a star formation prescription that is based on the rate at which gas generates entropy in shocks.”
• On the frequency, intensity, and duration of starburst episodes triggered by galaxy interactions and mergers (2008, methodology): “The evolution of the star formation rate in the Mice, studied by means of numerical simulations by Barnes (2004), also suggests star formation rates at most ten times greater than pre-interaction levels.”
• THE ROLE OF STARBURST–ACTIVE GALACTIC NUCLEUS COMPOSITES IN LUMINOUS INFRARED GALAXY MERGERS: INSIGHTS FROM THE NEW OPTICAL CLASSIFICATION SCHEME (2009, background): “Our future work includes integral field spectroscopy of composite galaxies and a detailed comparison between our results and the evolutionary merger models from numerical simulations Barnes (2004); Hopkins et al. (2005, 2006a,b, 2007, 2008).”
• Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies (2006, background): “Barnes (2004) has pointed out that current star formation recipes have a difficult time creating the starbursts observed in the shocked regions of merging galaxies, since star formation remains focused in the central regions of galaxies where the densities are high enough to facilitate star…”
• Feedback in simulations of disc-galaxy major mergers (2005, methodology): “Modeling of specific galaxy systems has already been done in several instances such as “The Mice” (Barnes 2004), M51 (Salo & Laurikainen 2000), Arp118 (Lamb et al. 1998), Arp119 (Hearn & Lamb 2001), Arp220 (McDowell et al. 2003), NGC 7714/15 (Struck & Smith 2003; Smith et al. 2005), NGC 2442 (Mihos…”
• Star formation in galaxy mergers with realistic models of stellar feedback and the interstellar medium (2012, background): “In contrast, it is well known that in models with a strong effective EOS, large density contrasts in shocks are poorly captured and so the SFR in these regions tends to be small, ∼10 per cent of the total (see Barnes 2004; Karl et al. 2010).”
• Formation of a Spiral Galaxy in a Major Merger (2004, background): “In the future, it may be possible to constrain these prescriptions by comparing the simulations with detailed observations, an approach beingpioneered by e.g. Barnes (2004) for the Mice.”
• GAS-PHASE OXYGEN GRADIENTS IN STRONGLY INTERACTING GALAXIES. I. EARLY-STAGE INTERACTIONS (2010, methodology): “These SPH/N-body simulations are described in detail in Barnes (2004).”
• THE ANTENNAE GALAXIES (NGC 4038/4039) REVISITED: ADVANCED CAMERA FOR SURVEYS AND NICMOS OBSERVATIONS OF A PROTOTYPICAL MERGER (2010, background): “Yet, it is limited by the large uncertainties imposed by our lack of understanding of the star-formation process (e.g., shock-induced vs. density-induced star formation, see Barnes 2004), the fraction of gas in the progenitors, etc.”
• HYDRODYNAMICS OF HIGH-REDSHIFT GALAXY COLLISIONS: FROM GAS-RICH DISKS TO DISPERSION-DOMINATED MERGERS AND COMPACT SPHEROIDS (2010, background): “Such modelling is required to reproduce correctly the extent of star formation in early- and late-stage interactions, which is missed by standard prescriptions (see also Barnes 2004; Chien & Barnes 2010).”
• Radial Variation of Attenuation and Star Formation in the Largest Late-Type Disks Observed with GALEX (2006, background): “It has also been recently suggested (Barnes 2004) that star formation may depend not only on the local gas density but may also be induced by shocks, especially in the case of interacting galaxies (we do not have such violently interacting systems in our sample).”
• A UNIVERSAL, LOCAL STAR FORMATION LAW IN GALACTIC CLOUDS, NEARBY GALAXIES, HIGH-REDSHIFT DISKS, AND STARBURSTS (2011, unknown): “…it is a crude approximation, and omits some of the complex physical processes that must take place in a merging or violently gravitationally unstable system, such as compressions produced by galaxy-scale shocks or inflows (Barnes 2004; Saitoh et al. 2010; Teyssier et al. 2010; Powell et al. 2011).”
• Detecting shock waves in cosmological smoothed particle hydrodynamics simulations (2006, methodology): “For example, when combined with radiative dissipation and star formation, our method can beused to study CR injection by supernova shocks, or to construct models for shock-induced star formation in the interstellar medium (e.g. Barnes 2004).”
• Star formation efficiency in galaxy interactions and mergers: a statistical study (2007, methodology): “It would be interesting also to perform a subset of these simulations varying the star formation rule, i.e. from a density-dependent Schmidt type one, to a formulation that could take into account energy dissipation in shocks, as proposed by Barnes (2004).”
• GALAXY MERGERS AND THE MASS–METALLICITY RELATION: EVIDENCE FOR NUCLEAR METAL DILUTION AND FLATTENED GRADIENTS FROM NUMERICAL SIMULATIONS (2010, methodology): “These simulations use the setup described in in §3.1 and Appendix A of Barnes (2004), except that ours exclude star formation.”
• SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS (2009, background): “Varying the hydrodynamical equation of state or the prescriptions for star formation or AGN activity can significantly change the detailed results (e.g., Barnes 2004; Cox et al. 2006).”