NR Peg: A new highly active semi-detached binary

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dc.contributor.authorErdem, A.
dc.contributor.authorSurgit, D.
dc.contributor.authorKurpinska-Winiarska, M.
dc.contributor.authorOblak, E.
dc.date.accessioned2025-01-27T20:41:49Z
dc.date.available2025-01-27T20:41:49Z
dc.date.issued2014
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractThis paper presents the first analysis of spectroscopic and photometric observations of the eclipsing binary star NR Peg. ELODIE H alpha observations indicate that the secondary component is a chromospherically active star; however, the spectral line profiles (especially of neutral metals) of NR Peg are very wide and have a complex structure with asymmetric bubbles on its branches, which could be interpreted as traces of stellar magnetic activity in both components. The 2007 and 2008 BVR light curves are generally those of beta Lyrae-type eclipsing binaries, however, there are large asymmetries between maxima. We explained these peculiar asymmetries in terms of large dark spots on the primary component. ELODIE spectroscopic data and 2008 BVR light curves were solved simultaneously using Wilson-Devinney code. The results describe NR Peg as a RS CVn type binary star with a semi-detached configuration. The masses of the components were found to be 1.60 +/- 0.03 M-circle dot, and 0.57 +/- 0.02 M-circle dot and the radii to be 3.35 +/- 0.07 R-circle dot and 3.55 +/- 0.08 R-circle dot for the primary and secondary components, respectively. Both components of NR Peg appear to have evolved behind the terminal age main sequence. However, the less-massive secondary component is significantly oversized and overluminous compared to theoretical evolution models. The distance of NR Peg was calculated as 138 +/- 12 pc, taking into account interstellar extinction, in agreement with the HIPPARCOS value. (C) 2014 Elsevier B.V. All rights reserved.
dc.description.sponsorshipCanakkale Onsekiz Mart University Research Foundation
dc.description.sponsorshipThis study was partly supported by Canakkale Onsekiz Mart University Research Foundation. We thank Mr. G.H. Lee and Ms. Inez Baranay for checking the English.
dc.identifier.doi10.1016/j.newast.2014.04.008
dc.identifier.endpage43
dc.identifier.issn1384-1076
dc.identifier.issn1384-1092
dc.identifier.scopus2-s2.0-84901346815
dc.identifier.scopusqualityQ2
dc.identifier.startpage38
dc.identifier.urihttps://doi.org/10.1016/j.newast.2014.04.008
dc.identifier.urihttps://hdl.handle.net/20.500.12428/24243
dc.identifier.volume33
dc.identifier.wosWOS:000337879500005
dc.identifier.wosqualityQ3
dc.indekslendigikaynakWeb of Science
dc.indekslendigikaynakScopus
dc.language.isoen
dc.publisherElsevier
dc.relation.ispartofNew Astronomy
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/closedAccess
dc.snmzKA_WoS_20250125
dc.subjectStars: binaries: eclipsing
dc.subjectStars: fundamental parameters
dc.subjectStars: individual (NR Peg)
dc.titleNR Peg: A new highly active semi-detached binary
dc.typeArticle

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