The peculiar chemical abundance of the transitional millisecond pulsar PSR J1023+0038-Li enhancement

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dc.contributor.authorShahbaz, T.
dc.contributor.authorGonzález-Hernández, J. I.
dc.contributor.authorBreton, R. P.
dc.contributor.authorKennedy, Mark R.
dc.contributor.authorSánchez, D. M.
dc.contributor.authorLinares, M.
dc.contributor.funderMinisterio de Ciencia e Innovaciónen
dc.contributor.funderEuropean Research Councilen
dc.contributor.funderIrish Research Councilen
dc.contributor.funderEuropean Regional Development Funden
dc.contributor.funderFundación Canaria de Investigación y Saluden
dc.date.accessioned2022-09-30T12:12:12Z
dc.date.available2022-09-30T12:12:12Z
dc.date.issued2022-03-02
dc.date.updated2022-09-30T11:56:42Z
dc.description.abstractUsing high-resolution optical spectroscopy we determine the chemical abundance of the secondary star in the binary millisecond pulsar PSR J1023+0038. We measure a metallicity of [Fe/H] = 0.48 ± 0.04 which is higher than the Solar value and in general find that the element abundances are different compared to the secondary stars in X-ray binaries and stars in the solar neighbourhood of similar Fe content. Our results suggest that the pulsar was formed in a supernova explosion. We find that supernova models, where matter that has been processed in the supernova is captured by the secondary star leading to abundance anomalies, qualitatively agree with the observations. We measure Li abundance of A(Li) = 3.66 ± 0.20, which is anomalously high compared to the Li abundance of stars with the same effective temperature, irrespective of the age of the system. Furthermore, the Li abundance in PSR J1023+0038 is higher than the Cosmic value and what is observed in young Population I stars and so provides unambiguous evidence for fresh Li production. The most likely explanation is the interaction of high-energy gamma-rays or relativistic protons from the pulsar wind or intrabinary shock with the CNO nuclei in the secondary star’s atmosphere via spallation which leads to substantial Li enrichment in the secondary star’s atmosphere.en
dc.description.sponsorshipMinisterio de Ciencia e Innovación, Spanish Ministry of Science and Innovation (MICINN project PID2020-114822GB-I00; MICINN project; PID2020-117493GB-I00; 2013 Ramon´ y Cajal program RYC-2013-14875); European Research Council (under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 715051; Spiders); (grant agreement No. 101002352)); Irish Research Council (Government of Ireland Postdoctoral Fellowship (GOIPD/2021/670: Invisible Monsters)); Fondo Europeo de Desarrollo Regional (FEDER) and the Canary Islands government (grant number PROID2020010104)en
dc.description.statusPeer revieweden
dc.description.versionPublished Versionen
dc.format.mimetypeapplication/pdfen
dc.identifier.citationShahbaz, T., González-Hernández, J.I., Breton, R.P., Kennedy, M.R., Sánchez, D.M. and Linares, M. (2022) ‘The peculiar chemical abundance of the transitional millisecond pulsar PSR J1023+0038 – Li enhancement’, Monthly Notices of the Royal Astronomical Society, 513(1), pp. 71–89. doi: 10.1093/mnras/stac492.en
dc.identifier.doi10.1093/mnras/stac492en
dc.identifier.endpage89en
dc.identifier.issn0035-8711
dc.identifier.issued1en
dc.identifier.journaltitleMonthly Notices of The Royal Astronomical Societyen
dc.identifier.startpage71en
dc.identifier.urihttps://hdl.handle.net/10468/13716
dc.identifier.volume513en
dc.language.isoenen
dc.publisherOxford University Pressen
dc.relation.urihttps://doi.org/10.1093/mnras/stac492
dc.rights© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Societyen
dc.subjectBinaries: Closeen
dc.subjectPulsars: Individual: PSR J1023+0038en
dc.subjectStars: Fundamental parametersen
dc.subjectStars: Individual: PSR J1023+0038en
dc.subjectStars: Neutronen
dc.subjectX-rays: Binariesen
dc.subject~Physics - Journal Articles~en
dc.titleThe peculiar chemical abundance of the transitional millisecond pulsar PSR J1023+0038-Li enhancementen
dc.typeArticle (peer-reviewed)en
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