REVIEW 4 cited by
Is the dust-to-gas ratio constant in molecular clouds?
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
abstract
We perform numerical simulations of dusty, supersonic turbulence in molecular clouds. We model 0.1, 1 and 10 {\mu}m sized dust grains at an initial dust-to-gas mass ratio of 1:100, solving the equations of combined gas and dust dynamics where the dust is coupled to the gas through a drag term. We show that, for 0.1 and 1 {\mu}m grains, the dust-to-gas ratio deviates by typically 10-20% from the mean, since the stopping time of the dust due to gas drag is short compared to the dynamical time. Contrary to previous findings, we find no evidence for orders of magnitude fluctuation in the dust-to-gas ratio for 0.1 {\mu}m grains. Larger, 10 {\mu}m dust grains may have dust-to-gas ratios increased by up to an order of magnitude locally. Both small (0.1 {\mu}m) and large ($\gtrsim$ 1 {\mu}m) grains trace the large-scale morphology of the gas, however we find evidence for 'size-sorting' of grains, where turbulence preferentially concentrates larger grains into dense regions. Size-sorting may help to explain observations of 'coreshine' from dark clouds, and why extinction laws differ along lines of sight through molecular clouds in the Milky Way compared to the diffuse interstellar medium.
Forward citations
Cited by 4 Pith papers
-
Using Scattered Near-Infrared Light to Map Water Ice in Prestellar Cores with SPHEREx
Coreshine SPHEREx spectra map 3 µm H2O ice across four prestellar cores; the two densest show an unexplained central drop in ice absorption that standard Bonnor-Ebert scattering models cannot reproduce.
-
Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster
In the Spiderweb protocluster, passive fraction rises with local density to ~60% while passive mass–size intercepts sit between field and cluster values, indicating advanced quenching but ongoing size growth.
-
Full one-fluid dusty gas with multiple grain species in SPH
Presents and benchmarks an SPH code for the full one-fluid dusty gas with multiple species that conserves mass, momentum, angular momentum and energy while recovering analytic solutions where the terminal velocity app...
-
Is the composition of the Solar atmosphere unusual, and if so, why? Possible interpretations
A review of the 10-20% solar volatile-to-refractory excess relative to solar twins, weighing galactic, protoplanetary, and planetary-ingestion explanations and finding no decisive answer.
Discussion (0). Continue with ORCID to comment.