Survival of Population III stars

Dutta, J.; Bagla, J.S.

Please use this identifier to cite or link to this item: http://hdl.handle.net/123456789/3472

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DC Field	Value	Language
dc.contributor.author	Dutta, J.	-
dc.contributor.author	Bagla, J.S.	-
dc.date.accessioned	2020-12-31T09:36:07Z	-
dc.date.available	2020-12-31T09:36:07Z	-
dc.date.issued	2020	-
dc.identifier.citation	Proceedings of the International Astronomical Union, 14, pp. 266 - 267.	en_US
dc.identifier.other	https://doi.org/10.1017/S1743921318007317	-
dc.identifier.uri	https://www.cambridge.org/core/journals/proceedings-of-the-international-astronomical-union/article/abs/survival-of-population-iii-stars/79E107B760144AD2E2AA1C95611D358A#article	-
dc.identifier.uri	http://hdl.handle.net/123456789/3472	-
dc.description	Only IISERM authors are available in the record.	-
dc.description.abstract	In 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.iso	en	en_US
dc.publisher	Cambridge University Press	en_US
dc.subject	stars: Pop III	en_US
dc.subject	Instabilities	en_US
dc.subject	Hydrodynamics	en_US
dc.subject	Accretion	en_US
dc.title	Survival of Population III stars	en_US
dc.type	Article	en_US
Appears in Collections:	Research Articles

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