Fundamental Parameters and Evolutionary Scenario of HD 327083
In this study, we present refined orbital and fundamental parameters of the Galactic B[e] supergiant binary system HD 327083 using the Bayesian Markov Chain Monte Carlo (MCMC) method applied to the radial velocities data of HD 327083. We found that the system is well described by a circular orbital...
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| Main Authors: | , , , , , |
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| Format: | Article |
| Language: | English |
| Published: |
MDPI AG
2025-04-01
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| Series: | Galaxies |
| Subjects: | |
| Online Access: | https://www.mdpi.com/2075-4434/13/3/47 |
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| Summary: | In this study, we present refined orbital and fundamental parameters of the Galactic B[e] supergiant binary system HD 327083 using the Bayesian Markov Chain Monte Carlo (MCMC) method applied to the radial velocities data of HD 327083. We found that the system is well described by a circular orbital model with the mass ratio of the components of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>q</mi><mo>=</mo><mn>1.15</mn><mo>±</mo><mn>0.07</mn></mrow></semantics></math></inline-formula>. We modeled the evolutionary history of the system using <span style="font-variant: small-caps;">MESA</span> code. Initially, the system was formed by a binary with the orbital period of <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mi>P</mi><mi>o</mi><mi>r</mi><mi>b</mi><mo>=</mo><mn>108</mn></mrow></semantics></math></inline-formula> day, which contained stars with 13.00 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mo>±</mo><mspace width="3.33333pt"></mspace><mn>0.05</mn></mrow></semantics></math></inline-formula> <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">M</mi><mo>⊙</mo></msub></semantics></math></inline-formula> and <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mn>11.50</mn><mo>±</mo><mn>0.05</mn></mrow></semantics></math></inline-formula> <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">M</mi><mo>⊙</mo></msub></semantics></math></inline-formula> masses. They had a relatively slow rotation <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><msub><mi>υ</mi><mrow><mi>r</mi><mi>o</mi><mi>t</mi></mrow></msub><mo>=</mo><mn>0.40</mn><mo>±</mo><mn>0.13</mn><msub><mi>υ</mi><mrow><mi>c</mi><mi>r</mi><mi>i</mi><mi>t</mi></mrow></msub></mrow></semantics></math></inline-formula> and provided a strong stellar wind. The current system age is <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><mrow><mn>13.6</mn><mo>±</mo><mn>0.1</mn></mrow></semantics></math></inline-formula> Myr, and the state of the system corresponds to a close filling of the high massive component’s Roche lobe and a beginning of the mass transfer. The mass-transfer event will occur in a short interval of ≲0.1 Myr only. After that, the mass of the post-primary drops to ≈5 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">M</mi><mo>⊙</mo></msub></semantics></math></inline-formula>, the post-secondary mass grows until ≈20 <inline-formula><math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><semantics><msub><mi mathvariant="normal">M</mi><mo>⊙</mo></msub></semantics></math></inline-formula>, and the binary will convert to a detached system with a long orbital period of ≈700 days. |
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| ISSN: | 2075-4434 |