The Disruption of Giant Molecular Clouds by Radiation Pressure and the Efficiency of Star Formation in Galaxies
arXiv:0906.5358 · doi:10.1088/0004-637X/709/1/191
Abstract
Star formation is slow, in the sense that the gas consumption time is much longer than the dynamical time. It is also inefficient; essentially all star formation in local galaxies takes place in giant molecular clouds (GMCs), but the fraction of a GMC converted to stars is very small, ~5%. In the most luminous starbursts, the GMC lifetime is shorter than the main sequence lifetime of even the most massive stars, so that supernovae can play no role in GMC disruption. We investigate the disruption of GMCs across a wide range of galaxies, from normal spirals to the densest starbursts; we take into account the effects of HII gas pressure, shocked stellar winds, protostellar jets, and radiation pressure produced by the absorption and scattering of starlight on dust grains. In the Milky Way, we find that a combination of three mechanisms, jets, HII gas pressure, and radiation pressure, disrupts the clouds. In more rapidly star forming galaxies such as ``clump'' galaxies at high-redshift, ultra-luminous infrared galaxies (ULIRGs) and submillimeter galaxies, radiation pressure dominates natal cloud distribution. We predict the presence of 10-20 clusters with masses ~10^7 Msun in local ULIRGs such as Arp 220 and a similar number of clusters with M_* ~ 10^8 Msun in high redshift clump galaxies; submillimeter galaxies will have even more massive clusters. We find that the mass fraction of a GMC that ends up in stars is an increasing function of the gas surface density of a galaxy, reaching ~35% in the most luminous starbursts. Furthermore, the disruption of bubbles by radiation pressure stirs the interstellar medium to velocities of ~10 km/s in normal galaxies and to ~100 km/s in ULIRGs like Arp 220, consistent with observations. Thus, radiation pressure may play a dominant role in the ISM of star-forming galaxies.
17 pages, 5 figures, submitted to ApJ
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- Comparing the Locations of Supernovae to CO (2-1) Emission in their Host Galaxies
- The formation of globular clusters with top-heavy initial mass functions
- Illuminating a tadpole's metamorphosis III: quantifying past and present environmental impact
- Discovery of a Very Large (~20 kpc) Galaxy at z=3.72
- On the Origin of the High Star-Formation Efficiency in Massive Galaxies at Cosmic Dawn
- A Tale of Two Clump Masses: A New Way to Study Clump Formation in Simulations
- Playing with FIRE: A Galactic Feedback-Halting Experiment Challenges Star Formation Rate Theories
- Turbulence and Star Formation in a Sample of Spiral Galaxies
- Faint AGN in z>~6 Lyman-break Galaxies Powered by Cold Accretion and Rapid Angular Momentum Transport
- Dust Eddington Ratios for Star-Forming Galaxy Subregions
- The THESAN-ZOOM project: Star formation efficiency from giant molecular clouds to galactic scale in high-redshift starbursts
- From Gas to Stars Over Cosmic Time
- Non-explosive pre-supernova feedback in the COLIBRE model of galaxy formation
- The Kelvin-Helmholtz instability in the Orion nebula: The effect of radiation pressure
- Photon Feedback: Screening and the Eddington Limit
- The life cycle of giant molecular clouds in simulated Milky Way-mass galaxies
- The Degeneracy of Galaxy Formation Models
- Magnetized Kelvin-Helmholtz instability in the presence of a radiation field
- The galaxy counterpart of the high-metallicity and 16 kpc impact parameter DLA towards Q0918+1636 - a challenge to galaxy formation models?
- Radiation Forces on Dust Envelopes
- Gas expulsion in MOND: the possible origin of diffuse globular clusters and ultra-faint dwarf galaxies
- Multi-scale simulations of black hole accretion in barred galaxies: Self-gravitating disk models
- Molecular gas properties in young stellar clusters with a suppressed star cluster wind
- Can molecular clouds live long?
- Exploring the evolution of a dwarf spheroidal galaxy with SPH simulations: II. AGN feedback
- The kinematics of star clusters undergoing gas expulsion in Newtonian and Milgromian dynamics
- Galactic chimney sweeping: the effect of 'gradual' stellar feedback mechanisms on the evolution of dwarf galaxies
- Galaxy formation hydrodynamics: From cosmic flows to star-forming clouds
- Characterising the z 7.66 Type-II AGN candidate SMACS S06355 using BEAGLE-AGN and JWST NIRSpec/NIRCam
- The origin and evolution of the [CII] deficit in HII regions and star-forming molecular clouds
- From Gas to Stars over Cosmic Time
- The Relative Importance of Thermal Gas, Radiation, and Magnetic Pressures Around Star-Forming Regions in Normal Galaxies and Dusty Starbursts
- The Arp 240 Galaxy Merger: A Detailed Look at the Molecular Kennicutt-Schmidt Star Formation Law on Sub-kpc Scales
- K-Band Imaging of the Nearby, Clumpy Turbulent Disk Galaxy DYNAMO G04-1
- Linking the Internal Properties of Infant Globular Clusters to their Formation Environments
- Ashes of FIRE: Modeling Dust Grain Size Evolution in the Local Group with FIRE
- The Star Formation Factory revisited I. The impact of metallicity on collapsing star-forming clouds
- Centrally concentrated star formation in young clusters
- Lyman- radiation pressure regulates star formation efficiency
- Radiation Pressure Feedback in Galaxies
- Capture and Escape: The Dependence of Radiation Forces on Clumping in Dusty Envelopes
- The Nun Path: The Evolution and Quenching of Satellite Galaxies
- Effect of dust rotational disruption by radiative torques on radiation pressure feedback from massive protostars