| 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 once clouds are marginally [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/SFHotConcepts#MagneticallyCritical magnetically critical], stars begin to form in earnest. However, this accounts for only a small portion of the cloud; about ~1% of the gas [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/SFHotConcepts#Starformationrateperlocalfreefalltime per local free-fall time] is turned into stars. This slow star formation takes place in only marginally supersonic condensations, suggesting that magnetic fields are primarily responsible for SF regulation, rather than turbulence (does this hold also for the gas that's '''not''' collapsing?). Notable figures [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/CFLitPaperFigures#MagneticallyRegulatedStarFormationinThreeDimensions:TheCaseoftheTaurusMolecularCloudComplex here], more notes [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/CFLitPaperNotes#MagneticallyRegulatedStarFormationinThreeDimensions:TheCaseoftheTaurusMolecularCloudComplex here][[br]] |
| | 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 stars begin to form once clouds are marginally [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/SFHotConcepts#MagneticallyCritical magnetically critical]. However, only a small portion of the nearly magnetically critical material is forming stars - about ~1% of the gas [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/SFHotConcepts#Starformationrateperlocalfreefalltime per local free-fall time]. The regulation of the SF in these regions seems to be due to magnetic fields rather than turbulence, as these regions are only marginally supersonic. Notable figures [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/CFLitPaperFigures#MagneticallyRegulatedStarFormationinThreeDimensions:TheCaseoftheTaurusMolecularCloudComplex here], more notes [https://astrobear.pas.rochester.edu/trac/wiki/u/erica/CFLitPaperNotes#MagneticallyRegulatedStarFormationinThreeDimensions:TheCaseoftheTaurusMolecularCloudComplex here][[br]] |
