Disc-halo interaction — I. Three-dimensional evolution of the Galactic disc

By M. D. Avillez. 2000

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The results of a three-dimensional model for disc–halo interaction are presented here. The model considers explicitly the input of energy and mass by isolated and correlated supernovae in the disc. Once disrupted by the explosions, the disc never returns to its initial state. Instead it approaches a state where a thin H i disc is formed in the Galactic plane, overlaid by thick H i and H ii gas discs with scaleheights of 500 pc and 1–1.5 kpc, respectively. The upper parts of the thick H ii disc (the diffuse ionized medium) act as a disc–halo interface, and its formation and stability are directly correlated to the supernova rate per unit area in the simulated disc.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cc69b87d9d9fcf32425e23b973301af7c5b2baf6

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Citations in the corpus

Global properties of the H I distribution in the outer Milky Way - Planar and extra-planar gas (2008, background): “Here we are interested in the steady state situation caused by dynamical processes as described e.g. by de Avillez (2000).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, background): “…are stratified boxes covering a statistically significant volume of the ISM with typical sizes (x×y×±z) of x = y ∼ 0.5−1 kpc, up to z ∼ ±20 kpc (de Avillez 2000; de Avillez & Berry 2001; de Avillez & Breitschwerdt 2004, 2005; Joung & Mac Low 2006; Piontek & Ostriker 2007; Joung, Mac Low…”
Mixing Timescales in a Supernova-driven Interstellar Medium (2002, methodology): “To study the mixing timescales in the ISM we added tracer fields to a modified version of the three-dimensional, SN-driven, ISM model of Avillez (2000).”
Towards simulating star formation in the interstellar medium (2004, methodology): “For isolated supernovae events, Avillez (2000) randomly determined the positions of supernovae in the disc plane with rates based on observed ones.”
Simulating the Formation of Molecular Clouds. II. Rapid Formation from Turbulent Initial Conditions (2006, background): “…& Inutsuka 2000, 2002; Bergin et al. 2004 ), or insufficient chemistry has been included to address the question at hand (e.g., Korpi et al. 1999; de Avillez 2000; Wada 2001; Kritsuk&Norman 2002a, 2002b, 2004; Balsara et al. 2004; de Avillez & Breitschwerdt 2004; Slyz et al. 2005; Joung & Mac Low…”
The Vertical Structure of Warm Ionised Gas in the Milky Way (2008, background): “At significant distances from the Galactic plane (z >∼ 2000 pc), theory predicts that>∼ 90% of the ISM by volume should be occupied by105 − 106 K coronal gas (Ferrière 1998b; Korpi et al. 1999; de Avillez 2000).”
Theoretical Challenges in Galaxy Formation (2016, methodology): “This behavior has already been reported by pioneering three-dimensional hydrodynamical simulations of stratified disks by Korpi et al. (1999), de Avillez (2000), de 32 Theoretical Challenges in Galaxy Formation Snapshots of the vertical gas column density distribution (top panels) and mid-plane…”
Interstellar Turbulence I: Observations and Processes (2004, background): “…& Norman 2001) and magnetic fields (Gazol-Patiño & Passot 1999) but are 2D, whereas others are 3D and either include the magnetic field with no self-gravity (Korpi et al. 1999a, Kim et al. 2001, Shukurov et al. 2004) or include neither field nor gravity (de Avillez 2000, de Avillez & Berry 2001).”
Turbulent Structure of a Stratified Supernova-driven Interstellar Medium (2005, methodology): “Avillez (2000) and Avillez & Berry (2001) used a stratified model similar to ours, but their studies focusedon the properties of a Galactic fountain in the Milky Way.”
Simulating the Formation of Molecular Clouds. I. Slow Formation by Gravitational Collapse from Static Initial Conditions (2006, background): “…properly treat the velocity field and often also include an approximate treatment of the thermal balance of the gas (e.g. Korpi et al. 1999; de Avillez 2000; Wada 2001; Kritsuk & Norman 2002a,b, 2004; Balsara et al. 2004; de Avillez & Breitschwerdt 2004; Slyz et al. 2005; Joung & Mac Low…”
The Supernova Rate-Velocity Dispersion Relation in the Interstellar Medium (2005, methodology): “…explosions models in the ISM have been presented in the literature (Rosen & Bregman 1995; Korpi et al. 1999a, 1999b; Gazol-Patiño & Passot 1999; de Avillez 2000; de Avillez & Berry 2001; Avila-Reese & Vázquez-Semadeni 2001; Kim et al. 2001; Kim 2004; de Avillez & Breitschwerdt 2004, 2005; Slyz…”
Volume filling factors of the ISM phases in star forming galaxies. I. The role of the disk-halo interaction (2004, methodology): “…work we report on large-scale simulations of the ISM including the disk and Galactic halo using a modified version of the SN driven ISM model of Avillez (2000) coupled to a three-dimensional HD code using adaptive mesh refinement (AMR) in a block-based structure, that relies on virtual…”
A High Spatial Resolution X-Ray and Hα Study of Hot Gas in the Halos of Star-forming Disk Galaxies. I. Spatial and Spectral Properties of the Diffuse X-Ray Emission (2003, background): “…of the ISM in normal spiral galaxies also predict hot gas in the halo, due to the interchange of material between the disk and halo through ‘‘galactic fountains’’ (Shapiro & Field 1976; Bregman 1980; de Avillez 2000), or in a more localized form through ‘‘chimneys’’ (Norman & Ikeuchi 1989).”
A High Spatial Resolution X-Ray and Hα Study of Hot Gas in the Halos of Star-forming Disk Galaxies. II. Quantifying Supernova Feedback (2003, background): “Second, multidimensional simulations of the ISM with energy return by SNe and stellar clusters show that bubbles do merge, and once merged they can potentially become powerful enough to escape the disk (de Avillez 2000).”
A dynamical model for the extraplanar gas in spiral galaxies (2005, background): “Other studies have concentrated on the modelling of the multiphase interstellar medium (ISM) (Rosen & Bregman 1995; de Avillez 2000), the cooling of the hot coronal gas (Corbelli & Salpeter 1988) and the effect of turbulence (Struck & Smith 1999).”
Toward First-Principle Simulations of Galaxy Formation: I. How Should We Choose Star-Formation Criteria in High-Resolution Simulations of Disk Galaxies? (2008, background): “In Runs B, C, and D, the disks appear rather clumpy, similarly to the results of threedimensional Eulerian simulations for galactic disk (e.g., de Avillez 2000a; de Avillez 2000b; Tasker & Bryan 2006; Wada & Norman 2007).”
Three-phase Interstellar Medium in Galaxies Resolving Evolution with Star Formation and Supernova Feedback (TIGRESS): Algorithms, Fiducial Model, and Convergence (2016, background): “…roles of SNe in driving turbulence and shaping the multiphase ISM in galactic disks have been extensively investigated (e.g., Korpi et al. 1999; de Avillez 2000; de Avillez & Breitschwerdt 2004; Joung & Mac Low 2006; Hill et al. 2012; Gent et al. 2013; Walch et al. 2015; Girichidis et al. 2016;…”
THE ROLE OF STELLAR FEEDBACK IN THE FORMATION OF GALAXIES (2007, background): “…(parsecs) to resolve the multiphase nature of the ISM and to explore complicated effects of stellar feedback on different scales (Rosen & Bregman 1995; Scalo et al. 1998; Korpi et al. 1999; de Avillez 2000; de Avillez & Breitschwerdt 2004, 2007; Wada & Norman 2001, 2007; Slyz et al. 2005).”