New photometric solutions of contact binaries HX UMa and FP Boo
[ X ]
Tarih
2023
Yazarlar
Dergi Başlığı
Dergi ISSN
Cilt Başlığı
Yayıncı
Elsevier
Erişim Hakkı
info:eu-repo/semantics/openAccess
Özet
By 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.
Açıklama
Anahtar Kelimeler
Binaries, Eclipsing -stars, Fundamental parameters -stars, Orbital period change -stars, Individuals (HX UMa and FP Boo)
Kaynak
New Astronomy
WoS Q Değeri
Q3
Scopus Q Değeri
Q2
Cilt
99
