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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7504
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dc.contributor.authorDutta, Jayanta-
dc.contributor.authorSur, Sharanya-
dc.contributor.authorStacy, Athena-
dc.contributor.authorBagla, Jasjeet Singh-
dc.date.accessioned2020-11-27T12:54:30Z-
dc.date.available2020-11-27T12:54:30Z-
dc.date.issued2018-05-
dc.identifier.citationProceedings of the International Astronomical Union, Vol. 342, pp. 266-267en_US
dc.identifier.issn1743-9213-
dc.identifier.urihttp://prints.iiap.res.in/handle/2248/7504-
dc.descriptionRestricted Access © International Astronomical Union https://doi.org/10.1017/S1743921318007317en_US
dc.description.abstractIn our earlier studyDutta (2016a), it has been shown that a number of primordial protostars (the ‘first stars’ in the Universe, also known as Population III or Pop III stars) are being ejected from the cluster of their origin with the velocity exceeding their escape velocity. Hence there is possibility that some of these protostars can enter main sequence and survive till present epoch, even in Milky Way. We ask the question if the protostars can avoid core collapse, and stop accreting before being ejected from the cluster, with the final mass of stars as 0.8 Mȯ.en_US
dc.language.isoenen_US
dc.publisherCambridge University Pressen_US
dc.relation.ispartofseriesIAU Symposium No. 342;-
dc.subjectstars: Pop IIIen_US
dc.subjectaccretionen_US
dc.subjecthydrodynamicsen_US
dc.subjectinstabilitiesen_US
dc.subjectmethods: numericalen_US
dc.titleSurvival of Population III starsen_US
dc.typeArticleen_US
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