Pemodelan Evolusi Sistem Bintang Ganda Tipe Algol Berbantuan MESA (Modules for Ekxperiments in Stellar Astrophysics) : Studi Kasus DN Orionis
Keywords:
Semi-detached binary, Roche Lobe Overflow (RLOF), Mass Transfer, Stellar Evolution, DN OrionisAbstract
The DN Orionis binary star system was a semi-detached binary undergoing mass transfer using Roche Lobe Overflow (RLOF) mechanism. This process played a role in the evolution of both stars, influencing physical parameters such as mass, radius, effective temperature, and orbital dynamics. This study aimed to analyze the impact of mass transfer on the evolution of both stars, focusing on changes in their parameters after the mass transfer ended without extending to their final evolutionary stages. Using MESA (Modules for Experiments in Stellar Astrophysics), the evolution of the DN Orionis system was modeled. Initially, the primary star had a smaller mass M = 1.8 Msun than the secondary M = 3.1 Msun, with an orbital period of P = 2.5 days. Mass transfer increased the primary’s mass to M = 2.9 Msun, while the secondary lost most of its mass, leaving M = 0.23 Msun. The radii and effective temperatures of both stars changed significantly: the secondary’s radius contracted from R = 5.67 Rsun to R = 0.0174 Rsun, while the primary expanded from R = 1.5 Rsun to R = 25.72 Rsun. The primary evolved into a sub-red giant with a effective temperature log Teff = 3.688, while the secondary became a white dwarf with a effective temperature log Teff = 4.2682. Angular momentum redistribution caused the orbital period to increase to P = 20.9 days. This study provided insights into how mass transfer shaped the evolution and parameters of semi-detached binary stars before reaching their final evolutionary stages, demonstrating that significant mass ratio inversion and orbital period expansion are key outcomes of Roche Lobe Overflow in systems like DN Orionis.
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