Thermal physics, cloud geometry and the stellar initial mass function

By R. Larson. 2005

281 citations recorded by the source corpus.

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In Astronomy and Astrophysics

Citations in the corpus

THE STELLAR INITIAL MASS FUNCTION IN EARLY-TYPE GALAXIES FROM ABSORPTION LINE SPECTROSCOPY. II. RESULTS (2012, background): “It has been argued that the characteristic mass scale and shape of the IMF is set by the Jeans mass (e.g., Larson 1998, 2005), by feedback from protostars (Silk 1995; Adams & Fatuzzo 1996; Krumholz 2011), or by the distribution of densities in a supersonically turbulent interstellar medium (Padoan…”
Spitzer Observations of Massive, Red Galaxies at High Redshift (2005, result): “As of yet there is no reason to expect the IMF to differ strongly from that observed in local galaxies (e.g., Baldry & Glazebrook 2003; Larson 2005), although some empirical studies and theoretical predictions suggest that a steeper IMF may be required in high-redshift massive starbursts (Ferguson…”
Is molecular gas necessary for star formation (2011, background): “73 proposed by Larson (1985, 2005).”
Can Supermassive Black Holes Form in Metal-enriched High-Redshift Protogalaxies? (2008, background): “Fragmentation Properties The thermal properties of star-forming clouds have an important influence on how they fragment into stars (Larson 2005).”
The Stellar IMF, Core Mass Function, & The Last-Crossing Distribution (2012, background): “…is a well-established result from both analytic work and numerical simulations (see e.g. Klessen & Burkert 2000, 2001; Bate & Bonnell 2005), and is true even if the gas is not isothermal (although our sub-sonic extrapolation is questionable in this case; see Larson 1985, 2005; Jappsen et al. 2005).”
The Large- and Small-Scale Structures of Dust in the Star-forming Perseus Molecular Cloud (2006, background): “Many theories have been put forth to account for the rough invariance of the slope including turbulent fragmentation (e.g., Padoan & Nordlund 2004), competitive accretion (e.g., Bonnell 2005), and thermal fragmentation (e.g., Larson 2005).”
Gravitational fragmentation and the formation of brown dwarfs in stellar clusters (2008, background): “The γ = 1.0 approximates the effect of dust cooling (Larson 2005) while the γ = 1.4 mimics the effects of when the collapsing core is optically thick to IR radiation, although its location at ρ = 5.5×10−15gcm−3, at lower densities than is typical, is in order to ensure that the Jeans mass is always…”
Dense gas in the Galactic central molecular zone is warm and heated by turbulence (2015, background): “…clouds (assuming TG,CMZ = 60 K, TG,local = 20 K, MJ,CMZ(n = 105cm−3) ≈ 9 M , MJ,local(n = 105cm−3) ≈ 2 M ); naively this implies a larger typical fragmentation scale and perhaps a preference toward forming high mass cores (Larson 2005), though the higher density in CMZ clouds should balance this.”
ERRATUM: “THE LUMINOSITY AND MASS FUNCTIONS OF LOW-MASS STARS IN THE GALACTIC DISK. II. THE FIELD” (2010, AJ, 139, 2679) (2010, background): “Larson (2005) suggested that thermal cooling arguments are also important in star formation.”
Radiative transfer and the energy equation in SPH simulations of star formation (2007, unknown): “For 10−18 g cm−3 <∼ ρ <∼ 10−13 g cm−3 we can approximate this with T ≃ 5 K [ ρ 10−18 g cm−3 ]0.08 (47) (cf. Larson 1973; Low & Lynden-Bell 1976; Masunaga & Inutsuka 2000; Larson 2005).”
SPIDER VIII - constraints on the stellar initial mass function of early-type galaxies from a variety of spectral features (2013, background): “…modelling point of view, the suggested change in the IMF of ETGs with velocity dispersion could be expected from the different physical properties of the star forming clouds during the formation of a massive galaxy (Larson 2005) – such as a turbulent ISM with a very high Mach number (Hopkins 2012).”
The initial conditions of star formation in the Ophiuchus main cloud: Kinematics of the protocluster condensations , (2007, background): “This strongly supports scenarios according to which the bulk of the IMF is at least partly determined by pre-collapse cloud fragmentation (e.g. Larson 1985, 2005; Elmegreen 1997; Padoan & Nordlund 2002).”
Radial variations in the stellar initial mass function of early-type galaxies (2014, background): “…thermal properties of the gas; the contribution of dust to cooling; magnetic fields; turbulence; the effect of supersonic motions in the turbulent gas; and the transition from pre-stellar cores to stars, among others (Padoan & Nordlund 2002; Larson 2005; Bonnell et al. 2008; Hopkins 2013).”
RADIATION-HYDRODYNAMIC SIMULATIONS OF THE FORMATION OF ORION-LIKE STAR CLUSTERS. II. THE INITIAL MASS FUNCTION FROM WINDS, TURBULENCE, AND RADIATION (2012, background): “Instead, models that seek to explain any characteristic mass scale in the IMF must appeal to departures from isothermality (Rees 1976; Low & Lynden-Bell 1976; Spaans & Silk 2000; Larson 2005; Krumholz 2011). ar X iv :1 20 3.”
The galaxy stellar mass-star formation rate relation: evidence for an evolving stellar initial mass function? (2007, background): “But a simple conjecture by Larson (1998, 2005) may have some empirical value.”
Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, background): “…IMF in starbursts remains controversial: though there are some theoretical reasons to believe that the IMF is more top-heavy in starbursts (e.g. Larson 1998, 2005; Elmegreen & Shadmehri 2003; Elmegreen 2004; Hopkins 2012; Narayanan & Davé 2012), there is to date no clear evidence for strong,…”
A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “…mass below which no cluster members exist; this limit would presumably correspond to mass of the smallest clumps in a cloud which can undergo thermal fragmentation (Low & Lynden-Bell 1976; Rees 1976; Spitzer 1978; Boss 2001; Larson 2005; Whitworth et al. 2007; see extended discussion in §4).”
Accretion-driven turbulence as universal process: galaxies, molecular clouds, and protostellar disks (2009, background): “…is the complex interplay between supersonic turbulence in the ISM and self-gravity in concert with magnetic fields, radiation, and thermal pressure that determines when and where stars form in the Galaxy (Mac Low & Klessen 2004; Larson 2005; Ballesteros-Paredes et al. 2007; McKee & Ostriker 2007).”
CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, background): “Possible examples include the physics of angular momentum retention in GRB progenitors (e.g., MacFadyen et al. 2001) or the effects of the cosmic background radiation temperature on the initial mass function (e.g., Larson 1998, 2005).”