Accelerating Star Formation in Clusters and Associations

By F. Palla, S. Stahler. 2000

225 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/41222643079ac58bf2fed39584c0de8b70c39df1

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Citations in the corpus

The Initial Configuration of Young Stellar Clusters: A K-Band Number Counts Analysis of the Surface Density of Stars (2004, background): “…than or on the order of 105 to 106 yr to allow for a significant frequency of interactions to occur over the length of a forming star’s protostellar collapse phase (Kenyon & Hartmann 1995) or the approximate length of a young cluster’s active star–forming phase (Palla & Stahler 2000), respectively.”
Equilibrium Star Cluster Formation (2006, background): “Palla & Stahler (2000) found formation times for Taurus-Auriga, Lupus, Chamaeleon, Upper Scorpius, and NGC 2264 that are & 3 Myr, but the first three of these are not rich clusters, Upper Scorpius has undergone too much dynamical spreading to reliably estimate its dynamical time at formation, and…”
2MASS Observations of the Perseus, Orion A, Orion B, and Monoceros R2 Molecular Clouds (2000, background): “If the Palla & Stahler (2000) model is correct, most molecular clouds should not contain a substantial stellar population since they are relatively dormant for most of their cloud lifetimes.”
TRANSITIONAL DISKS AS SIGNPOSTS OF YOUNG, MULTIPLANET SYSTEMS (2011, background): “…a high scattering timescale limit of 5 × 105 years, which is one-half to one-quarter the estimated stellar age in the Taurus-Auriga association (Palla & Stahler 2000) and five times higher than the inferred transitional disk lifetime/clearing time (Furlan et al. 2009), we find that the gap…”
On the Rapid Collapse and Evolution of Molecular Clouds (2007, background): “If star formation accelerates in a cloud core (Palla & Stahler 2000), then the average stellar mass fraction during the lifetime of the core is less than half of the final mass fraction, and the core duration would be less than 2.75 Myr.”
Stellar rotation and variability in the Orion Nebula Cluster (2002, background): “Palla & Stahler (2000), for example, propose that the observations favor an acceleration of star formation with time.”
Accretion Rates in Herbig Ae stars (2006, background): “HAe stars are, on average, older than Ophiuchus objects, which cluster at ages∼ 0.5 − 1 Myr, respectively (Palla & Stahler 2000).”
Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood (2001, methodology): “While one can find small numbers of “older” stars in all these regions, the results of Palla & Stahler (2000) show that these do not imply significant star formation rates.”
The formation of a bound star cluster: from the orion nebula cluster to the pleiades (2000, background): “In reality, stars appear to continue forming in a cluster for a few Myr until the gas is expelled (Palla & Stahler 2000), and once a star forms it decouples from the gas and either falls towards the potential minimum or is already on a “virial equilibrium orbit”.”
A Spitzer Census of the IC 348 Nebula (2007, background): “The interpretation of such a “peak” depends upon the accurate counting of the population of embedded protostars, which could not be included into previous studies of cluster age spreads (e.g. Palla & Stahler 2000) as they lacked the deep mid-IR data provided by Spitzer 22.”
Control of star formation by supersonic turbulence (2000, result): “…by BallesterosParedes et al. (1999), then the long star formation timescale computed here is quite consistent with the very low star formation efficiencies seen in Taurus (e.g. Leisawitz et al. 1989, Palla & Stahler 2000, Hartmann 2001), as the cloud simply has not had time to form many stars.”
TOWARD A COMPLETE ACCOUNTING OF ENERGY AND MOMENTUM FROM STELLAR FEEDBACK IN GALAXY FORMATION SIMULATIONS (2012, background): “…clump lifetime tcl is a highly uncertain factor, but can reasonably be assumed to be a fixed multiple of the clump crossing time: tcl = Nctc with Nc ∼ 5 − 10 (Palla & Stahler 2000), where crossing time tc is given by tc≡ Rh σ = C3/2R√ 0.4G M(α−1)/2cl , (A14) where R = CR Mαcl relation was…”
Flows, Fragmentation, and Star Formation. I. Low-Mass Stars in Taurus (2002, background): “If one adopts the estimate that the average age of the Taurus stars is ∼ 2 Myr (Palla & Stahler 2000), and that molecular clouds in the solar neighborhood disperse after a timescale of order 4 Myr or less (HBB), it is possible that Taurus is only about halfway through forming stars; in this case the”
Photoevaporation of protoplanetary discs - II. Evolutionary models and observable properties (2006, methodology): “The inner disc begins to drain at t = 6.01 Myr, and the disc is cleared to the outer grid radius (2500 au) at t = 6.20 Myr.”
Global hierarchical collapse in molecular clouds. Towards a comprehensive scenario (2019, background): “…exists for the acceleration of star formation, either from the presence of tails of old-age stars in the age histograms in young, embedded clusters (Palla & Stahler 1999, 2000; Da Rio et al. 2010), or by the more numerous and more centrally concentrated nature of the younger members of a cluster…”
Slow Star Formation in Dense Gas: Evidence and Implications (2006, methodology): “Finally, note that there are few star clusters where one can estimate the star formation rate directly by placing a large number of stars on the HR diagram and using preYmain-sequence tracks to estimate the cluster mass and age spread (e.g., Palla & Stahler 1999, 2000; Huff & Stahler 2006).”