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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7887
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dc.contributor.authorDutta, Jayanta-
dc.date.accessioned2022-02-10T05:20:01Z-
dc.date.available2022-02-10T05:20:01Z-
dc.date.issued2015-12-15-
dc.identifier.citationAstrophysics and Space Science, 2016, Vol. 361, Article No. 35en_US
dc.identifier.issn0004-640X-
dc.identifier.issn1572-946X (Online)-
dc.identifier.urihttp://hdl.handle.net/2289/7887-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en_US
dc.description.abstractIt is generally believed that angular momentum is distributed during the gravitational collapse of the primordial star forming cloud. However, so far there has been little understanding of the exact details of the distribution. We use the modified version of the Gadget-2 code, a three-dimensional smoothed-particle hydrodynamics simulation, to follow the evolution of the collapsing gas in both idealized as well as more realistic minihalos. We find that, despite the lack of any initial turbulence and magnetic fields in the clouds the angular momentum profile follows the same characteristic power-law that has been reported in studies that employed fully self-consistent cosmological initial conditions. The fit of the power-law appears to be roughly constant regardless of the initial rotation of the cloud. We conclude that the specific angular momentum of the self-gravitating rotating gas in the primordial minihalos maintains a scaling relation with the gas mass as L ∝ M^{1.125}. We also discuss the plausible mechanisms for the power-law distribution.en_US
dc.language.isoenen_US
dc.publisherSpringeren_US
dc.relation.urihttps://ui.adsabs.harvard.edu/abs/2016Ap%26SS.361...35D/abstracten_US
dc.relation.urihttps://arxiv.org/abs/1512.01656en_US
dc.relation.urihttp://dx.doi.org/10.1007/s10509-015-2622-yen_US
dc.rights2016 Springeren_US
dc.subjectstar formationen_US
dc.subjectearly universeen_US
dc.subjecthydrodynamicsen_US
dc.subjectinstabilitiesen_US
dc.titleAngular momentum distribution during the collapse of primordial star-forming cloudsen_US
dc.typeArticleen_US
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