Volume filling factors of the ISM phases in star forming galaxies. I. The role of the disk-halo interaction

By M. A. D. A. D. Breitschwerdt. 2004

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The role of matter circulation between the disk and halo in establishing the volume filling factors of the different ISM phases in the Galactic disk (|z |≤ 250 pc) is investigated, using a modified version of the three-dimensional supernova- driven ISM model of Avillez (2000). We carried out adaptive mesh refinement simulations of the ISM with five supernova rates (in units of the Galactic value), σ/σGal = 1, 2, 4, 8 and 16 (corresponding to starburst conditions) using three finer level resolutions of 2.5, 1.25 and 0.625 pc, allowing us to understand how resolution would affect the volumes of gas phases in pressure equilibrium. We find that the volume filling factors of the different ISM phases depend sensitively on the existence of a duty cycle between the disk and halo acting as a pressure release valve for the hot (T > 10 5.5 K) phase in the disk. The amount of cold gas (defined as the gas with T < 10 3 K) picked up in the simulations varies from a value of 19% for σ/σGal = 1 to ∼5% for σ/σGal = 4a nd≤1% for higher SN rates. Background heating prevents the cold gas from immediate collapse and thus ensures the stability of the cold gas phase. The mean occupation fraction of the hot phase varies from about 17% for the Galactic SN rate to ∼28%, for σ/σGal = 4, and to 44% for σ/σGal = 16. Overall the filling factor of the hot gas does not increase much as we move towards higher SN rates, following a power law offv, hot �∝ (σ/σGal) 0.363 . Such a modest dependence on the SN rate is a consequence of the evacuation of the hot phase into the halo through the duty cycle. This leads to volume filling factors of the hot phase considerably smaller than those predicted in the three-phase model of McKee & Ostriker (1977) even in the absence of magnetic fields.

Subfields: Astronomy and Astrophysics, Instrumentation

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TOWARD A COMPLETE ACCOUNTING OF ENERGY AND MOMENTUM FROM STELLAR FEEDBACK IN GALAXY FORMATION SIMULATIONS (2012, background): “…ISM by regulating star formation (Mac Low & Klessen 2004; McKee & Ostriker 2007, and references therein), driving turbulence (Kim et al. 2001; de Avillez & Breitschwerdt 2004; Joung & Mac Low 2006; Agertz et al. 2009a; Tamburro et al. 2009) and generating galactic scale outflows (Martin 1999,…”
Theoretical Challenges in Galaxy Formation (2016, background): “Theoretical Challenges in Galaxy Formation 33 Avillez & Breitschwerdt (2004), and Joung & Mac Low (2006).”
MOMENTUM INJECTION BY SUPERNOVAE IN THE INTERSTELLAR MEDIUM (2014, background): “…to play the predominant role in creating the hot phase and shaping the large-scale structure of the multiphase ISM (e.g., Norman & Ikeuchi 1989; de Avillez & Breitschwerdt 2004; Hill et al. 2012; Hennebelle & Iffrig 2014), in driving turbulence in diffuse gas (e.g., Rosen & Bregman 1995; Mac Low…”
Clump morphology and evolution in MHD simulations of molecular cloud formation (2008, background): “…and temperature ranges, which has been suggested to be in transit between the stable warm and cold phases (Vázquez-Semadeni et al. 2000; Gazol et al. 2001; SánchezSalcedo et al. 2002; Vázquez-Semadeni et al. 2003; de Avillez & Breitschwerdt 2004; Gazol et al. 2005; Audit & Hennebelle 2005).”
Toward First-Principle Simulations of Galaxy Formation: I. How Should We Choose Star-Formation Criteria in High-Resolution Simulations of Disk Galaxies? (2008, background): “…have been a number of studies on this issue (e.g., Vazquez-Semadeni 1994; Scalo et al. 1998; VázquezSemadeni et al. 2000; Wada 2001; de Avillez & Mac Low 2002; Kravtsov 2003; de Avillez & Breitschwerdt 2004; Slyz et al. 2005; Wada & Norman 2007; Tasker & Bryan 2007; Robertson & Kravtsov 2007).”
Physical Processes in the Interstellar Medium (2014, background): “Note, however, that substantial motions only lasted about 1 Myr after a heating event (Kritsuk & Norman, 2002b; de Avillez & Breitschwerdt, 2004, 2005, 2007).”
Simulating the Formation of Molecular Clouds. II. Rapid Formation from Turbulent Initial Conditions (2006, background): “…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 2006).”
Turbulent Structure of a Stratified Supernova-driven Interstellar Medium (2005, methodology): “…extremely hot diffuse gas in the halo has very long cooling timestcool(n) = 51/n−3 Myr, where n−3 ≡ n/(10−3cm−3), if we take the cooling rate at T = 106K. Avillez & Breitschwerdt (2004a) ran a similar model for a much longer period (400 Myr) and showed that aftert ≈ 70 Myr the statistical…”
The SILCC project - III. Regulation of star formation and outflows by stellar winds and supernovae (2016, background): “They investigate the structure of the ISM that is stirred by SN feedback (e.g. de Avillez & Breitschwerdt 2004, 2007; Joung & Mac Low 2006; Joung, Mac Low & Bryan 2009; Hill et al. 2012; Shetty & Ostriker 2012; Kim, Ostriker & Kim 2013), with self-gravity (Gent et al. 2013a,b; Hennebelle & Iffrig…”
VERTICAL STRUCTURE OF A SUPERNOVA-DRIVEN TURBULENT, MAGNETIZED INTERSTELLAR MEDIUM (2012, methodology): “Note that the evolved picture seen here as well as in similar, recent work (e.g., Avillez & Breitschwerdt 2004; JM06) is one of a pervasive, warm intercloud medium with embedded supernova remnants and superbubbles.”
Simulating the Formation of Molecular Clouds. I. Slow Formation by Gravitational Collapse from Static Initial Conditions (2006, background): “…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 2006) have not previously included sufficient chemistry to follow the formation of H2…”
Three-phase Interstellar Medium in Galaxies Resolving Evolution with Star Formation and Supernova Feedback (TIGRESS): Algorithms, Fiducial Model, and Convergence (2016, background): “…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; Li et al. 2017).”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, background): “Both de Avillez & Breitschwerdt (2004, 2005) and Hill et al. (2012) emphasize that time-scales of a few hundred Myr are needed for a fountain cycle to establish a global dynamical equilibrium and a converged vertical profile of the stratified disc.”
THE ROLE OF STELLAR FEEDBACK IN THE FORMATION OF GALAXIES (2007, methodology): “This is roughly consistent with ISM simulations with a 1 pc resolution (de Avillez & Breitschwerdt 2004), Galactic ISM models and observations (Ferrière 1998).”
The Supernova Rate-Velocity Dispersion Relation in the Interstellar Medium (2005, background): “…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 et al. 2005; Mac Low et al. 2005).”
MORPHOLOGICAL QUENCHING OF STAR FORMATION: MAKING EARLY-TYPE GALAXIES RED (2009, background): “The cross-section given to gas particles ensures about one collision per particle and per vertical crossing time and corresponds to a filling factor in spiral disks of about 5%, which can be realistic for the ISM (de Avillez & Breitschwerdt 2004).”