Star formation from the small to the large scale

By F. Favata, A. A. Kaas, Alyson G. Wilson. 2000

205 citations recorded by the source corpus.

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The Tumultuous Lives of Galactic Dwarfs and the Missing Satellites Problem (2004, background): “We find that c = 10 is a best fit to the abundance and radial distribution of the Local Group galaxies (see §6.2).”
Astrophysical and cosmological information from large-scale submillimetre surveys of extragalactic sources (2007, methodology): “These include a simple merger model, a hydrodynamical model, the stable clustering model by Hughes & Gaztañaga (2000), and a phenomenological model.”
A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “…of a number of additional faint satellite galaxies (Willman et al. 2005; Irwin et al. 2007; Liu et al. 2008; Martin et al. 2008; Simon & Geha 2007; Grebel 2000; van den Bergh 2000; Belokurov et al. 2008; Watkins et al. 2009; Belokurov et al. 2010), there remains a considerable discrepancy between…”
Theoretical isochrones in several photometric systems. II. The Sloan Digital Sky Survey ugriz system (2004, unknown): “It illustrates that Aλ has a very small, non-linear trend with AV (see also Grebel & Roberts 1995). The RV = 5.0 value, suitable for dense star-forming regions as the Orion Nebulae, is also considered. In this case, Aλ/AV ratios become very different from the previous ones. Most of Table 1 is dedica”
The stellar halo of the Galaxy (2008, methodology): “(1996) used very deep HST counts of M dwarfs and obtained a factor four smaller number of red dwarfs, in agreement with Gould et al. (1998) who find ρ0 ∼ 6.”
Dark Matter Subhalos and the Dwarf Satellites of the Milky Way (2008, result): “Let us assume that the observed dSphs are fossils of this first generation of small-mass galaxies, a hypothesis consistent with the fact that old populations with ages > 10 Gyr are the dominant stellar component of Milky Way dSphs (see e.g. Grebel 2000; Dolphin et al. 2005).”
The Reionization of the Universe by the First Stars and Quasars (2000, background): “At high redshift it may be biased toward massive, efficiently ionizing stars (e.g., Abel, Bryan, & Norman 2000; Bromm, Coppi, & Larson 1999), but this remains very much uncertain.”
Complexity on Small Scales: The Metallicity Distribution of the Carina Dwarf Spheroidal Galaxy (2005, background): “All dSphs (and all other dwarfs) studied in sufficient detail so far have been shown to contain ancient populations that are indistinguishable in age with the oldest age-datable populations in the Milky Way (Grebel 2000, Grebel & Gallagher 2004).”
High-Mass Protostellar Candidates. I. The Sample and Initial Results (2001, background): “Progress reports on this project were presented earlier by Menten et al. (1999), Sridharan et al. (1999), and Beuther et al. (2000).”
Observing the Dark Matter Density Profile of Isolated Galaxies (2003, methodology): “No halos outside the regions of high resolution are used in our analysis.”
The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. I. Results from 19 OB Associations in the Magellanic Clouds (2000, result): “Such short timescales for star formation are consistent with recent studies by Elmegreen (1997, 2000a, 2000b), who argues that star formation takes place not over 10 of crossing times but over one or two.”
The initial conditions of star formation in the Ophiuchus main cloud: Kinematics of the protocluster condensations , (2007, background): “As pointed out by Clark et al. (2007), if the lifetime of the condensations depends on their mass, then the observed mass spectrum is not necessarily representative of the intrinsic condensation mass distribution (CMD) (see also Elmegreen 2000).”
Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood (2001, background): “Moreover, Ballesteros-Paredes (1999, 2000) has shown that even if there is equipartition be- tween the kinetic, magnetic and gravitational energy components (Ballesteros-Paredes & VázquezSemadeni 1995, 1997), the kinetic energy term (pressure) does not necessarily contribute support against…”
On the Initial Mass Function of Population III Stars (2000, background): “This discrepancy seems to come from most studies being restricted to highly simplified models such as homogeneous, pressureless, and/or spherical collapses.”
The physics of star formation (2003, background): “…on the problem, no mechanism has yet been identified that is clearly capable of providing the desired outward transport of angular momentum, but some of the possibilities have been reviewed by Larson (1989), Adams and Lin (1993), Papaloizou and Lin (1995), Stahler (2000), and Stone et al (2000).”