Photoionizing feedback in star cluster formation

By J. Dale, Ian A. Bonnell, C. Clarke, Matthew R. Bate. 2005

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We present the first ever hydrodynamic calculations of star cluster formation that incorporate the effect of feedback from ionizing radiation. In our simulations, the ionizing source forms in the cluster core at the intersection of several dense filaments of inflowing gas. We show that these filaments collimate ionized outflows and suggest such an environmental origin for at least some observed outflows in regions of massive star formation. Our simulations show both positive feedback (i.e. promotion of star formation in neutral gas compressed by expanding H ii regions) and negative feedback (i.e. suppression of the accretion flow in to the central regions). We show that the volume filling factor of ionized gas is very different in our simulations from the result from the case where the central source interacted with an azimuthally smoothed gas density distribution. As expected, gas density is the key parameter in determining whether or not clusters are unbound by photoionizing radiation. Nevertheless, we find – on account of the acceleration of a small fraction of the gas to high velocities in the outflows – that the deposition in the gas of an energy that exceeds the binding energy of the cluster is not a sufficient criterion for unbinding the bulk of the cluster mass.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/8726f0b11798f76b15940e8f1e9d1c71290e0e3a

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Citations in the corpus

Astrophysical smooth particle hydrodynamics (2009, methodology): “For the various approaches we refer to the literature (Navarro and White, 1993; Mihos and Hernquist, 1994; Bate et al., 1995, 2003; Gerritsen and Icke, 1997; Sommer-Larsen et al., 1999; Springel, 2000, 2005; Springel et al., 2001; Thacker and Couchman, 2000; Scannapieco et al., 2001; Thacker et al.,”
Massive stars in massive clusters II: Disruption of bound clusters by photoionization (2012, background): “Dale et al. (2005) and Dale & Bonnell (2011) found that accretion flows onto the O–stars strongly limit the effect of radiation by only allowing it to escape into a small fraction of the sky as seen from each source.”
The SILCC (SImulating the LifeCycle of molecular Clouds) project – I. Chemical evolution of the supernova-driven ISM (2014, background): “Stars E-mail: walch@ph1.uni-koeln.de form in many of these clouds and exert strong feedback on the surrounding gas, in the form of UV radiation (Dale et al. 2005; Dale, Ercolano & Bonnell 2012; Walch et al. 2012, 2013), stellar winds (Toalá & Arthur 2011; Rogers & Pittard 2013), and supernova (SN)…”
The SILCC (SImulating the LifeCycle of molecular Clouds) project - II. Dynamical evolution of the supernova-driven ISM and the launching of outflows (2015, unknown): “Numerical studies support this paradigm and show efficient heating of the surroundings by OB stars (Dale et al. 2005; Peters et al. 2010; Arthur et al. 2011; Walch et al. 2012; Dale et al. 2014; Geen et al. 2015).”
LIMITING ACCRETION ONTO MASSIVE STARS BY FRAGMENTATION-INDUCED STARVATION (2010, methodology): “The reason for this behavior is that the star formation process is controlled by the local Jeans mass, which depends to a large degree on how the filaments in the disk shield the radiation (compare Section 3.2), as previously noted by Dale et al. (2005, 2007) and Krumholz et al. (2009).”
Physical Processes in the Interstellar Medium (2014, background): “They can also influence the molecular cloud material that surrounds Ralf Klessen & Simon Glover 89 the young star cluster (e.g. Dale et al., 2005; Dale & Bonnell, 2011; Walch et al., 2012, 2013).”
Dispersal of molecular clouds by ionizing radiation (2012, background): “The effect of ionsation feedback has been explored numericlly by Dale et al. (2005).”
WHAT DRIVES THE EXPANSION OF GIANT H ii REGIONS?: A STUDY OF STELLAR FEEDBACK IN 30 DORADUS (2010, background): “…an HII shell (Thompson et al. 2005; Murray et al. 2010b; Andrews & Thompson 2011), the warm gas ionized by massive stars (e.g., Whitworth 1979; Dale et al. 2005), the hot gas shock heated by stellar winds and supernovae (e.g., Yorke et al. 1989; Harper-Clark & Murray 2009), and protostellar…”
Before the first supernova: combined effects of H II regions and winds on molecular clouds (2014, unknown): “Dale et al. (2005) observed a similar effect operating within HIIRs in the absence of winds.”
A sub-parsec resolution simulation of the Milky Way: global structure of the interstellar medium and properties of molecular clouds (2013, background): “A debate still exists on the exact role of radiative feedback in preventing, and/or triggering star formation, and in modifying the inner structure of clouds (see Dale et al. 2005; Dale & Bonnell 2011; Tremblin et al. 2012, and references therein).”
On the fraction of star formation occurring in bound stellar clusters (2012, background): “This might not actually hold once the first supernovae have started to inject energy into the ISM, as the heating might either prevent or stimulate some regions from undergoing collapse (Elmegreen & Lada 1977; Dale et al. 2005; Wünsch et al. 2008).”
Star formation through gravitational collapse and competitive accretion (2006, background): “Even the intrinsically isotropic feedback from high-mass stars escapes in preferential directions due to the non-uniform gas distributions (Dale et al. 2005; Krumholz et al. 2005c).”
Evidence for top-heavy stellar initial mass functions with increasing density and decreasing metallicity (2012, background): “This is likely to be an oversimplification (Dale et al. 2005).”
Theory of Star Formation (2007, background): “High star formation efficiencies are possible in a clump with embedded H II regions since their destructive effect is significantly reduced in a clump composed of dense cores (Tan & McKee, 2001; Dale et al., 2005).”
H II REGIONS: WITNESSES TO MASSIVE STAR FORMATION (2010, background): “Dale et al. (2005) performed the first hydrodynamic calculation of a star cluster forming region to include a simplified treatment of ionization feeback, but only from a single source that was inserted into a pre-existing simulation and whose ionizing flux did not depend on the mass of the growing…”
Equilibrium Star Cluster Formation (2006, background): “This is consistent with observations that massive stars are not always the last to form in their clusters (e.g. Eisenhauer et al. 1998; Hoogerwerf et al. 2001), and theoretical work showing that clumpiness greatly inhibits gas dispersal (Tan & McKee 2004; Dale et al. 2005).”
The Global Evolution of Giant Molecular Clouds. I. Model Formulation and Quasi-Equilibrium Behavior (2006, unknown): “However, to date only preliminary attempts to solve the problem have been made (e.g. Dale et al. 2005; Mellema et al. 2005; Mac Low et al. 2006; Krumholz et al. 2006b), so we are forced to rely an analytic approximations.”