The Formation of Stars

By S. Stahler, F. Palla. 2005

301 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/6fcf7a6e30ad755ce2c65cef792aacced942ed51

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In Astronomy and Astrophysics

Citations in the corpus

Accretion disks in luminous young stellar objects (2015, methodology): “The pre-main-sequence evolutionary tracks used to estimate the location of the birthline and M? are from Stahler & Palla (2005).”
The RMS Survey: Ammonia and water maser analysis of massive star forming regions. ⋆ (2011, background): “Ammonia is an excellent tracer of high-density gas (∼104 cm−3; Evans 1999; Stahler & Palla 2005), and is relatively unaffected by depletion at lower temperatures compared to other common molecular tracers such as CO (Bergin & Langer 1997).”
Spectral imaging of the Central Molecular Zone in multiple 3-mm molecular lines (2011, background): “…transfer equation has the general solution for the intensity of a velocity channel in a spectral line known as the detection equation (e.g. Stahler & Palla 2005): TA = T ∗ A/η = f [Jν (Tex)− Jν(TBG)](1− exp(−τν)) whereT ∗A is the measured intensity,η the extended beam efficiency (taken as…”
Effect of episodic accretion on the structure and the lithium depletion of low-mass stars and planet-hosting stars (2010, background): “Proto lowmass stars below about 2M⊙ are expected to be entirely convective (Stahler & Palla 2005).”
Clustered and Triggered Star Formation in W5: Observations with Spitzer (2008, methodology): “We make use of this by measuring αIR (see, e.g. Lada 1987; Stahler & Palla 2005): αIR = d log (λFλ) d log λ (1) the value of which decreases with the progression of the star’s evolutionary state, whether through its own aging, or the effects of its environment.”
The coronal X-ray - age relation and its implications for the evaporation of exoplanets (2011, background): “Early in the life of the star before it reaches the main sequence this is evidently no true and PMS stars have significantly higher luminosities than their MS counterparts (see e.g. Stahler & Palla 2005).”
On the self-enrichment scenario of galactic globular clusters: constraints on the IMF (2006, background): “…to an extreme degree by internal nucleosynthesis (i.e. the [O/Na] ratio in the ejecta is invariably -1.4); II-c) The time-scale of the evolution of the polluters is shorter than the formation time-scale of the low-mass stars (0.1-0.8 M⊙), i.e. shorter than about 100 Myr (Stahler & Palla 2005).”
Broad-band non-thermal emission from molecular clouds illuminated by cosmic rays from nearby supernova remnants (2009, background): “The typical density of a cloud is of about few hundred atoms per cubic centimeter, but much higher densities can be found in less massive and smaller (parsec or sub-parsec scale) molecular cloud cores, dark clouds or Bok globules (see Stahler and Palla 2005, for a review).”
The big problems in star formation: The star formation rate, stellar clustering, and the initial mass function (2014, background): “While there are several textbooks on star formation (Stahler & Palla 2005; Ward-Thompson & Whitworth 2011; Bodenheimer 2011; Schulz 2012), this material is not part of the standard graduate curriculum at most institutions, and there is little material available that bridges the gap between a…”
Star Formation in the Milky Way and Nearby Galaxies (2012, background): “…leads to the formation of a first hydrostatic core in a small region where the dust continuum emission becomes optically thick; this short-lived core is still molecular and grows in mass by continued infall from the outer layers (Larson 1969; Boss & Yorke 1995; Omukai 2007; Stahler & Palla 2005).”