New photometric solutions of contact binaries HX UMa and FP Boo

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dc.contributor.authorYildirim, M. F.
dc.date.accessioned2025-01-27T21:01:49Z
dc.date.available2025-01-27T21:01:49Z
dc.date.issued2023
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractBy using different databases (TESS, SuperWASP, KWS and ASAS-SN), light curve analyzes of HX UMa and FP Boo systems were performed, and the changes in the orbital period of the systems were also examined. The light curve analyzes of the systems were conducted simultaneously with the radial velocities using the Wilson and Devinney (WD) code. As a result of the analyzes, the masses and radii of the components were determined as M1 = 1.29 +/- 0.02 M AE, M2 = 0.38 +/- 0.02 M AE, R1 = 1.21 +/- 0.02 R AE, R2 = 0.78 +/- 0.02 R AE for HX UMa and M1 = 1.68 +/- 0.05 M AE, M2 = 0.16 +/- 0.01 M AE, R1 = 2.28 +/- 0.02 R AE, R2 = 0.82 +/- 0.02 R AE for FP Boo, respectively. The distances of HX UMa and FP Boo were calculated as 123 +/- 11 pc and 350 +/- 23 pc, respectively, and were almost the same as Gaia DR3 values. When the orbital period changes were examined, it was determined that the orbital period of the HX UMa system increased, while the FP Boo decreased. The orbital period increase rate of HX UMa was calculated as dP/dt = 9 x 10-8 d yr-1 and the period decrease rate of FP Boo was calculated as dP/dt = 1.7 x 10-6 d yr-1. Mass transfer between components has been suggested as the reason for the period changes. Along with the orbital period changes, a cyclical change was observed in both systems. Magnetic activity or a possible third component can cause cyclical variation. The periods of these cyclical changes are determined as 24 +/- 4 yr and 20 +/- 1 yr, respectively.
dc.identifier.doi10.1016/j.newast.2022.101946
dc.identifier.issn1384-1076
dc.identifier.issn1384-1092
dc.identifier.scopus2-s2.0-85139987252
dc.identifier.scopusqualityQ2
dc.identifier.urihttps://doi.org/10.1016/j.newast.2022.101946
dc.identifier.urihttps://hdl.handle.net/20.500.12428/27196
dc.identifier.volume99
dc.identifier.wosWOS:000878788400004
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/openAccess
dc.snmzKA_WoS_20250125
dc.subjectBinaries
dc.subjectEclipsing -stars
dc.subjectFundamental parameters -stars
dc.subjectOrbital period change -stars
dc.subjectIndividuals (HX UMa and FP Boo)
dc.titleNew photometric solutions of contact binaries HX UMa and FP Boo
dc.typeArticle

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