1,388 research outputs found
Turbulent Formation of Interstellar Structures and the Connection Between Simulations and Observations
I review recent results derived from numerical simulations of the turbulent
interstellar medium (ISM), in particular concerning the nature and formation of
turbulent clouds, methods for comparing the structure in simulations and
observations, and the effects of projection of three-dimensional structures
onto two dimensions. Clouds formed as turbulent density fluctuations are
probably not confined by thermal pressure, but rather their morphology may be
determined by the large-scale velocity field. Also, they may have shorter
lifetimes than normally believed, as the large-scale turbulent modes have
larger associated velocities than the clouds' internal velocity dispersions.
Structural characterization algorithms have started to distinguish the best
fitting simulations to a particular observation, and have opened several new
questions, such as the nature of the observed line width-size relation and of
the relation between the structures seen in channel maps and the true spatial
distribution of the density and velocity fields. The velocity field apparently
dominates the morphology seen in intensity channel maps, at least in cases when
the density field exhibits power spectra steep enough. Furthermore, the
selection of scattered fluid parcels along the line of sight (LOS) by their
LOS-velocity inherent to the construction of spectroscopic data may introduce
spurious small-scale structure in high spectral resolution channel maps.Comment: 15 pages, no figures. To appear in the Proceedings of "The Chaotic
Universe", Roma/Pescara, Italy, 1-5 Feb. 1999, eds. V. Gurzadyan and L.
Bertone. Uses included .cls fil
Dependence of the Star Formation Efficiency on the Parameters of Molecular Cloud Formation Simulations
We investigate the response of the star formation efficiency (SFE) to the
main parameters of simulations of molecular cloud formation by the collision of
warm diffuse medium (WNM) cylindrical streams, neglecting stellar feedback and
magnetic fields. The parameters we vary are the Mach number of the inflow
velocity of the streams, Msinf, the rms Mach number of the initial background
turbulence in the WNM, and the total mass contained in the colliding gas
streams, Minf. Because the SFE is a function of time, we define two estimators
for it, the "absolute" SFE, measured at t = 25 Myr into the simulation's
evolution (sfeabs), and the "relative" SFE, measured 5 Myr after the onset of
star formation in each simulation (sferel). The latter is close to the "star
formation rate per free-fall time" for gas at n = 100 cm^-3. We find that both
estimators decrease with increasing Minf, although by no more than a factor of
2 as Msinf increases from 1.25 to 3.5. Increasing levels of background
turbulence similarly reduce the SFE, because the turbulence disrupts the
coherence of the colliding streams, fragmenting the cloud, and producing
small-scale clumps scattered through the numerical box, which have low SFEs.
Finally, the SFE is very sensitive to the mass of the inflows, with sferel
decreasing from ~0.4 to ~0.04 as the the virial parameter in the colliding
streams increases from ~0.15 to ~1.5. This trend is in partial agreement with
the prediction by Krumholz & McKee (2005), since the latter lies within the
same range as the observed efficiencies, but with a significantly shallower
slope. We conclude that the observed variability of the SFE is a highly
sensitive function of the parameters of the cloud formation process, and may be
the cause of significant scatter in observational determinations.Comment: 19 pages, submitted to MNRA
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