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Differential abundance analysis of Procyon and θ Sculptoris: Comparison with abundance patterns of solar‐like pairs
dc.contributor.authorCowley, Charles R.
dc.contributor.authorYüce, Kutluay
dc.contributor.authorBord, Donald J.
dc.date.accessioned2020-03-17T18:29:43Z
dc.date.availableWITHHELD_11_MONTHS
dc.date.available2020-03-17T18:29:43Z
dc.date.issued2020-01
dc.identifier.citationCowley, Charles R.; Yüce, Kutluay ; Bord, Donald J. (2020). "Differential abundance analysis of Procyon and θ Sculptoris: Comparison with abundance patterns of solar‐like pairs." Astronomische Nachrichten 341(1): 125-132.
dc.identifier.issn0004-6337
dc.identifier.issn1521-3994
dc.identifier.urihttps://hdl.handle.net/2027.42/154353
dc.description.abstractThe precision differential abundance (PDA) technique is applied to the mid‐F stars Procyon and θ Scl using spectra from the ESO UVESPOP library. We relate PDA patterns to endogenous processes related to condensation or to exogenous processes connected to Galactic chemical evolution. We employ one‐dimensional LTE models, but emphasize the use of weaker lines (≤20 mÅ) that are typically used in such studies. We compare our results with PDAs of solar‐type stars. Abundances and PDAs are determined for 28 elements: C, N, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Cu, Zn, Y, Zr, Ba, La, Ce, Nd, Sm, Eu, and Gd. A plot of PDAs (θ Scl minus Procyon) versus Z shows a highly significant correlation. Moreover, local substructure of the plot for the elements Ca‐Zn and neutron‐addition elements is similar to that which can be found for solar twins. Our PDA versus Z plot structural shows similarity to plots that can be made from the extensive work of Bedell et al. (2018). That PDA structure and substructure is clearly a function of age.
dc.publisherWILEY‐VCH Verlag GmbH & Co. KGaA
dc.subject.otherstars: abundances — stars: solar‐type — stars: individual: Procyon — stars: individual: θ Scl
dc.titleDifferential abundance analysis of Procyon and θ Sculptoris: Comparison with abundance patterns of solar‐like pairs
dc.typeArticle
dc.rights.robotsIndexNoFollow
dc.subject.hlbsecondlevelAstronomy
dc.subject.hlbtoplevelScience
dc.description.peerreviewedPeer Reviewed
dc.description.bitstreamurlhttps://deepblue.lib.umich.edu/bitstream/2027.42/154353/1/asna202013694.pdf
dc.description.bitstreamurlhttps://deepblue.lib.umich.edu/bitstream/2027.42/154353/2/asna202013694_am.pdf
dc.identifier.doi10.1002/asna.202013694
dc.identifier.sourceAstronomische Nachrichten
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dc.owningcollnameInterdisciplinary and Peer-Reviewed


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