TIC 236653616: A Long-Period Eclipsing Binary Candidate Comprising a Sun-like Star and a low-mass late-type Companion

Öz

This study presents a detailed photometric characterization of TIC 236653616, identified as a detached eclipsing binary system using high-cadence data from TESS Sector 83. Initial periodogram analysis via the Box Least Squares algorithm suggested a 10.04-day cycle; however, phase-folding and differentiation between primary (10.334%) and secondary (9.297%) eclipse depths confirmed a true orbital period of 20.0872 days. To ensure the astrophysical nature of the signal, rigorous vetting procedures were applied, including centroid analysis which yielded a PRF fit quality of 0.995, and an Even-Odd consistency check that ruled out instrumental false positives (1.10). The system parameters were derived using a Bayesian framework incorporating a quadratic limb darkening model. Markov Chain Monte Carlo simulations converge on a high-inclination orbit (i ≈ 88.3°) consisting of a Sun-like primary star (R1 ≈ 1.05 R⊙) and a secondary M-dwarf binary companion (R2 ≈ 0.33 R⊙). These results provide a robust orbital solution and a high-fidelity baseline for future radial velocity studies to determine the absolute masses of the components.

Anahtar Kelimeler

• Eclipsing Binaries
• Photometry
• TESS
• MCMC
• Stellar Parameters

TIC 236653616: Güneş benzeri bir yıldız ile düşük kütleli, geç tip bir eş yıldızdan oluşan uzun periyotlu bir tutulmalı ikili yıldız adayı

Öz

Bu çalışma, TESS Sektör 83 verileri kullanılarak TIC 236653616 sisteminin fotometrik analizini ve örten çift yıldız olarak karakterizasyonunu sunmaktadır. Box Least Squares (BLS) algoritması ile yapılan ilk incelemeler 10.04 günlük bir periyoda işaret etse de, evreye katlama analizi sonucunda birincil (%10.334) ve ikincil (%9.297) tutulma derinliklerinin ayrışmasıyla gerçek yörünge periyodunun 20.0872 gün olduğu saptanmıştır. Sinyalin astrofiziksel kökenini doğrulamak amacıyla uygulanan centroid vetting analizi 0.995 PRF uyum kalitesiyle sinyalin hedef yıldızdan geldiğini kanıtlamış, Even-Odd testi ise enstrümantal hata olasılığını (1.10) dışlamıştır. Sistemin fiziksel parametreleri, kuadratik kenar kararması (limb darkening) modelini içeren Bayesian yaklaşımı ve Markov Chain Monte Carlo simülasyonları ile hesaplanmıştır. Elde edilen sonuçlar, 88.3° eğime sahip bir yörüngede dolanan Güneş benzeri bir ana kol yıldızı (R1 ≈ 1.05 R⊙) ve bir M-cüce bileşenden (R2 ≈ 0.33 R⊙) oluşan kararlı bir sistem konfigürasyonunu ortaya koymaktadır. Bu çalışma, bileşenlerin mutlak kütlelerinin belirlenmesi için gelecekte yapılacak radyal hız (radial velocity) gözlemleri için hassas bir temel oluşturmaktadır.

Anahtar Kelimeler

• Örten Çift Yıldızlar
• Yıldız Parametreleri
• Fotometri
• TESS
• MCMC

Kaynakça

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