Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/8521
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dc.contributor.authorPal, Harshit-
dc.contributor.authorSubramaniam, A-
dc.contributor.authorReddy, A. B. S-
dc.contributor.authorJadhav, Vikrant V-
dc.date.accessioned2024-08-30T05:04:46Z-
dc.date.available2024-08-30T05:04:46Z-
dc.date.issued2024-08-01-
dc.identifier.citationThe Astrophysical Journal Letters, Vol. 970, No. 2, L39en_US
dc.identifier.issn2041-8205-
dc.identifier.urihttp://hdl.handle.net/2248/8521-
dc.descriptionOpen Accessen_US
dc.descriptionOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.-
dc.description.abstractWe report the discovery of a barium blue straggler star (BSS) in M67, exhibiting enhancements in slow neutron-capture (s-)process elements. Spectroscopic analysis of two BSSs (WOCS 9005 & WOCS 1020) and four stars located near the main-sequence turn-off using GALAH spectra, showed that WOCS 9005 has a significantly high abundance of the s-process elements ([Ba/Fe] = 0.75 ± 0.08, [Y/Fe] = 1.09 ± 0.07, and [La/Fe] = 0.65 ± 0.06). The BSS (WOCS 9005) is a spectroscopic binary with a known period, eccentricity, and a suspected white dwarf (WD) companion with a kinematic mass of 0.5 M⊙. The first "sighting" of the WD in this barium BSS is achieved through multiwavelength spectral energy distribution (SED) with the crucial far-UV data from the UVIT/AstroSat. The parameters of the hot and cool companions are derived using binary fits of the SED using two combinations of models, yielding a WD with Teff in the range 9750–15,250 K. Considering the kinematic mass limit, the cooling age of the WD is estimated as ∼60 Myr. The observed enhancements are attributed to a mass transfer (MT) from a companion asymptotic giant branch star, now a WD. We estimate the accreted mass to be 0.15 M⊙, through wind accretion, which increased the envelope mass from 0.45 M⊙. The detection of chemical enhancement, as well as the sighting of WD in this system, have been possible due to the recent MT in this binary, as suggested by the young WD.en_US
dc.language.isoenen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.3847/2041-8213/ad6316-
dc.rights© 2024. The Author(s)-
dc.subjectOpen star clustersen_US
dc.subjectBarium starsen_US
dc.subjectBlue straggler starsen_US
dc.subjectWhite dwarf starsen_US
dc.subjectS-processen_US
dc.subjectSpectroscopic binary starsen_US
dc.subjectSpectral energy distributionen_US
dc.titleDiscovery of a Barium Blue Straggler Star in M67 and “Sighting” of Its White Dwarf Companionen_US
dc.typeArticleen_US
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