A Guide to Comparisons of Star Formation Simulations with Observations

@article{Goodman2010AGT,
  title={A Guide to Comparisons of Star Formation Simulations with Observations},
  author={Alyssa A. Goodman},
  journal={Proceedings of the International Astronomical Union},
  year={2010},
  volume={6},
  pages={511 - 519}
}
  • A. Goodman
  • Published 1 May 2010
  • Physics
  • Proceedings of the International Astronomical Union
Abstract We review an approach to observation-theory comparisons we call “Taste-Testing.” In this approach, synthetic observations are made of numerical simulations, and then both real and synthetic observations are “tasted” (compared) using a variety of statistical tests. We first lay out arguments for bringing theory to observational space rather than observations to theory space. Next, we explain that generating synthetic observations is only a step along the way to the quantitative… 

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References

SHOWING 1-10 OF 44 REFERENCES

A Theory of the IMF for Star Formation in Molecular Clouds

We present models for the initial mass function (IMF) for stars forming within molecular clouds. These models use the idea that stars determine their own masses through the action of powerful stellar

THE KINEMATICS OF MOLECULAR CLOUD CORES IN THE PRESENCE OF DRIVEN AND DECAYING TURBULENCE: COMPARISONS WITH OBSERVATIONS

In this study, we investigate the formation and properties of prestellar and protostellar cores using hydrodynamic self-gravitating adaptive mesh refinement simulations, comparing the cases where

The "True" Column Density Distribution in Star-Forming Molecular Clouds

We use the COMPLETE Survey's observations of the Perseus star-forming region to assess and intercompare the three methods used for measuring column density in molecular clouds: near-infrared (NIR)

THE INTERPLAY OF TURBULENCE AND MAGNETIC FIELDS IN STAR-FORMING REGIONS: SIMULATIONS AND OBSERVATIONS

We analyze a suite of thin-sheet magnetohydrodynamical simulations based on the formulation of Basu, Ciolek, Dapp, and Wurster. These simulations allow us to examine the observational consequences to

On the relative motions of dense cores and envelopes in star-forming molecular clouds

Hydrodynamical simulations of star formation indicate that the motions of protostars through their natal molecular clouds may be crucial in determining the properties of stars through competitive

Physical versus Observational Properties of Clouds in Turbulent Molecular Cloud Models

We examine the question of how well the physical properties of clumps in turbulent molecular clouds can be determined by measurements of observed clump structures. To do this, we compare simulated

A role for self-gravity at multiple length scales in the process of star formation

A ‘dendrogram’ (hierarchical tree-diagram) analysis reveals that self-gravity plays a significant role over the full range of possible scales traced by 13CO observations in the L1448 molecular cloud, but not everywhere in the observed region.

The structure of molecular clouds and the universality of the clump mass function

Using a smoothed particle hydrodynamics (SPH) simulation of a star-forming region in a molecular cloud, we show that the emergence of a clump mass function (CMF) resembling the stellar initial mass

The Efficiency of Grain Alignment in Dense Interstellar Clouds: a Reassessment of Constraints from Near-Infrared Polarization

We present the results of a detailed study of interstellar polarization efficiency (as measured by the ratio pλ/τλ) toward molecular clouds, with the aim of discriminating between grain alignment

2MASS wide field extinction maps III. The Taurus, Perseus, and California cloud complexes

We present a near-infrared extinction map of a large region in the sky (∼3500 deg 2 ) in the general directions of Taurus, Perseus, and Aries. The map has been obtained using robust and optimal