V1130 Cyg ve V461 Lyr Örten Çift Sistemlerinin Sergilediği Aktivitenin Doğası

Abstract

Bu çalışmada, ``The Challenges of Modelling the Activities Occurring on Eclipsing Binaries V1130 Cyg and V461 Lyr'' başlıklı "Revista Mexicana de Astronomia y Astrofisica Vol. 57, pp. 335-349 (2021)" künyeli makalemizin geniş Türkçe özeti sunulacaktır ve hedef sistemlerin Kepler Uydusu ile elde edilen verilerinin analiz sonuçlarını içermektedir. (O-C)II artıklarının incelenmesiyle özellikle V461 Lyr'in sergilediği kromosferik aktivite etkisinin oldukça baskın olduğu görülmüştür. V1130 Cyg için 94 flare, V461 Lyr için 255 flare tespit edilmiştir. Flareler OPEA modeli olarak tanımlanan modelleme yöntemi ile kromosferik aktivitenin doyma seviyesi belirlenmiş ve istatistiksel yöntemler, literatürden farklı olarak V1130 Cyg flarelerinin iki, V461 Lyr flarelerinin ise üç farklı OPEA modeli ile modellenmesi gerektiğini göstermiştir. Ayrıca, V1130 Cyg göç dönemi 0.34 yıl olan tek lekeye, V461 Lyr dört lekeye sahiptir. V461 Lyr sisteminin bileşenlerinin iki lekesi aynı bileşen üzerinde olacak şekilde göç dönemleri 11.58 yıl ve 10.59 yıl, diğer bileşen üzerindeki 11.81 yıl ve 12.84 yıl olarak bulunmuştur.

Keywords

• techniques: photometric
• methods: data analysis
• methods: statistical
• binaries: eclipsing
• stars: low-mass
• stars: flare
• stars: individual (V461 Lyr)
• stars: individual (V1130 Cyg)

Nature of Activity Exhibited by Eclipsing Binaries V1130 Cyg and V461 Lyr

Abstract

In this study, an extensive Turkish summary of our article titled "The Challenges of Modeling the Activities Occurring on Eclipsing Binaries V1130 Cyg and V461 Lyr" with the tag "Revista Mexicana de Astronomia y Astrofisica Vol. 57, pp. 335-349 (2021)" will be presented and It contains the analysis results of the data of the target systems obtained with the Kepler Satellite. By examining the (O-C)II residues, it was seen that the chromospheric activity effect, especially that exhibited by V461 Lyr, was quite dominant. 94 flares were detected for V1130 Cyg and 255 flares for V461 Lyr. The saturation level of chromospheric activity was determined with the modeling method defined as the flares OPEA model, and statistical methods showed that, unlike the literature, V1130 Cyg flares should be modeled with two different OPEA models and V461 Lyr flares should be modeled with three different OPEA models. Additionally, V1130 Cyg has a single spot with a migration period of 0.34 years, while V461 Lyr has four spots. The migration periods of the components of the V461 Lyr system were found to be 11.58 years and 10.59 years, with two spots on the same component, and 11.81 years and 12.84 years on the other component.

Keywords

• techniques: photometric
• methods: data analysis
• methods: statistical
• binaries: eclipsing
• stars: low-mass
• stars: flare
• stars: individual (V461 Lyr)
• stars: individual (V1130 Cyg)

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