| 3 | | '''[http://adsabs.harvard.edu/abs/2008ApJ...687..354N Magnetically Regulated Star Formation in Three Dimensions: The Case of the Taurus Molecular Cloud Complex], ''Nakamura, Fumitaka; Li, Zhi-Yun'' '''[[br]] Model strong fields + diffuse clouds, motivated by observations of Taurus & Pipe Nebula which show large scale ordered fields that run perpendicular to diffuse elongated clouds. Sims include ambipolar diffusion and outflow feedback. Find that ~1% of the magnetically critical gas is turned into stars per local free-fall time. This slow star formation takes place in only marginally supersonic condensations, suggesting that magnetic fields are primarily responsible for SF regulation, rather than turbulence. Notable figures [[https://astrobear.pas.rochester.edu/trac/wiki/u/erica/CFLitPaperFigures here]]. |
| | 3 | '''[http://adsabs.harvard.edu/abs/2008ApJ...687..354N Magnetically Regulated Star Formation in Three Dimensions: The Case of the Taurus Molecular Cloud Complex], ''Nakamura, Fumitaka; Li, Zhi-Yun'' '''[[br]] Model strong fields + diffuse clouds, motivated by observations of Taurus & Pipe Nebula which show large scale ordered fields that run perpendicular to diffuse elongated clouds. Sims include ambipolar diffusion and outflow feedback. Find that ~1% of the magnetically critical gas is turned into stars per local free-fall time. This slow star formation takes place in only marginally supersonic condensations, suggesting that magnetic fields are primarily responsible for SF regulation, rather than turbulence. Notable figures [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/CFLitPaperFigures#MagneticallyRegulatedStarFormationinThreeDimensions:TheCaseoftheTaurusMolecularCloudComplex here]. |
