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Fluorine detection in hot extreme helium stars

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dc.contributor.author Bhowmick, A
dc.contributor.author Pandey, G
dc.contributor.author Lambert, D. L
dc.date.accessioned 2021-02-14T06:40:35Z
dc.date.available 2021-02-14T06:40:35Z
dc.date.issued 2020-12
dc.identifier.citation Journal of Astrophysics and Astronomy, Vol. 41, No. 1, 40 en_US
dc.identifier.issn 0250-6335
dc.identifier.uri http://hdl.handle.net/2248/7655
dc.description © Indian Academy of Sciences https://doi.org/10.1007/s12036-020-09659-2 en_US
dc.description The original publication is available at springerlink.com
dc.description.abstract The origin and evolution of hydrogen-deficient stars are not yet adequately understood. Their chemical peculiarities, along with hydrogen-deficiency, makes them stand out from the rest and sheds light on their possible origin. Severe fluorine enrichment (of the order of 800–8000) is one such characteristic feature of a class of hydrogen deficient stars, mainly the RCBs (R Coronae Borealis stars) and cool EHes (Extreme Helium stars) which enforces their close connection. For hot EHes, this relationship with the cooler EHes, based on their fluorine abundance is unexplored. Here, first estimates of fluorine abundances in hot EHes are presented and discussed in the light of their cooler counterparts to try to establish an evolutionary connection. The relation between these fluorine estimates with the other elemental abundances observed in these stars plays a pivotal role to predict the formation and evolution of these exotic stars. en_US
dc.language.iso en en_US
dc.publisher Springer en_US
dc.subject Hydrogen-deficient stars en_US
dc.subject chemical peculiarity en_US
dc.subject cxtreme helium stars en_US
dc.title Fluorine detection in hot extreme helium stars en_US
dc.type Article en_US

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