Molecular Depletion and Thermal Balance in Dark Cloud Cores

By Paul F. Goldsmith. 2000

356 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/1b1c5f0425a29b5065db004bbd535f94bf47fce5

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Citations in the corpus

On The Internal Structure Of Starless Cores. Physical and Chemical Properties of L1498 and L1517B (2004, unknown): “4 shows, a model with the “standard” cosmic ray ionization rate of ζ = 3× 10−17 s−1 (Goldsmith 2001), overestimates the core temperature at all radii (in fact, it overestimates the (2, 2) intensity by more than a factor of 2).”
Accretion disks in luminous young stellar objects (2015, background): “However, if dust and gas are not perfectly coupled, then Td can differ by a few degrees from the temperature estimated of the high-density tracers (Goldsmith, 2001; Juvela & Ysard, 2011).”
Systematic Molecular Differentiation in Starless Cores (2001, background): “…5.5), and given that the central densities we derive ( 105 cm 3) are high enough for gas and dust to be thermally coupled (Goldsmith &Langer 1978; Goldsmith 2001), we conclude that if central cooling is present, it occurs at scales smaller than the resolution of our molecular line data, so it…”
Hierarchical fragmentation and differential star formation in the Galactic ‘Snake’: infrared dark cloud G11.11−0.12 (2014, methodology): “These structures are dense enough that gas and dust are well coupled (Goldsmith 2001), thus we use the NH3 gas temperature as a direct measure of the dust temperature throughout this paper.”
CO Isotopologues in the Perseus Molecular Cloud Complex: the X-factor and Regional Variations (2008, methodology): “It is important to note that almost all the points lie below the median dust temperature of the region, indicating that 12CO is tracing gas at volume densities well below 105 cm 3, the lower limit to have dust and gas coupling (Goldsmith 2001).”
Dense gas in the Galactic central molecular zone is warm and heated by turbulence (2015, background): “This is generally a good assumption on the scales we observe, as typical gas cooling rates via line or dust cooling around TG ∼ 100 K and n ∼ 105cm−3 are dT/dt ∼ 10−20erg s−1cm−3 ∼ 23(n/105cm−3)K kyr−1 (Goldsmith 2001, and see below).”
The molecular gas in Luminous Infrared Galaxies I: CO lines, extreme physical conditions, and their drivers (2011, background): “…line cooling for self-gravitating gas iwellapproximated by the expression: Λline = 1.9× 10−27n ( Tkin 10K )3 erg cm−3 s−1 (16) (Papadopoulos 2010 and references therein), with most of itdue to the CO SLEDs though other molecules (e.g.13CO) significantly contribute when n&104 cm−3 (Goldsmith 2001).”
A general model for the CO–H2 conversion factor in galaxies with applications to the star formation law (2011, background): “When the gas densities are 104 cm−3, the dust and gas exchange energy efficiently, and the gas temperature approaches the dust temperature (Goldsmith 2001; Juvela & Ysard 2011).”
Evolution of Chemistry and Molecular Line Profiles during Protostellar Collapse (2004, background): “However, Goldsmith (2001) and Doty & Neufeld (1997) found the effects of depletion of CO and evaporation of water were relatively small at high densities because of efficient gas-dust coupling.”
Modelling CO formation in the turbulent interstellar medium (2009, background): “…temperatures, but would also have to take into account several other physical processes that are not included in our current model, such as the freeze-out of CO and water onto dust grains, or the fact that the dust temperature in the cloud will decrease as the extinction increases (Goldsmith 2001).”
THE EFFECT OF LINE-OF-SIGHT TEMPERATURE VARIATION AND NOISE ON DUST CONTINUUM OBSERVATIONS (2009, background): “Though the dust mass is only a fraction of the gas mass (∼ 1/100), gas temperatures may also exhibit gradients, due to the coupling between dust and gas at high enough densities (Goldsmith 2001; Crapsi et al. 2007).”
Is molecular gas necessary for star formation (2011, background): “However, we do not expect this simplification to significantly affect the thermal balance of the cloud (see e.g. Goldsmith 2001).”
Our astrochemical heritage (2012, background): “This is the critical density for gas cooling by gas-dust collisions (Goldsmith 2001) and it represents the “dividing line” for dynamical stability.”
THE PdBI ARCSECOND WHIRLPOOL SURVEY (PAWS). I. A CLOUD-SCALE/MULTI-WAVELENGTH VIEW OF THE INTERSTELLAR MEDIUM IN A GRAND-DESIGN SPIRAL GALAXY (2013, methodology): “5gas with ∆ T = Tgas − Tdust (Goldsmith 2001).”
THE RELATION BETWEEN GAS AND DUST IN THE TAURUS MOLECULAR CLOUD (2010, background): “The kinetic temperature in dense regions is likely to be in between 5 and 10K (Goldsmith 2001) and therefore, assuming that the isotopologues are thermalized, the excitation temperature should also have a value in this range.”
Cold Dark Clouds: The Initial Conditions for Star Formation (2007, background): “The detailed study of thermal balance in dense cores by Goldsmith (2001) shows that the gas-dust coupling, together with the high efficiency of the dust radiative cooling, easily compensates the disappearance of molecular coolants, and keeps the temperature of the gas deep inside the core at rather…”