Study of Eclipsing Binary and Multiple Systems in OB Associations V: MQ Cen in Crux OB1
| Autor: | Miloslav Zejda, Selçuk Bilir, Hicran Bakiş, Jan Janík, Jiří Liška, Zdeněk Mikulášek, Volkan Bakiş, Christian Nitschelm, Efecan Tunc |
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| Rok vydání: | 2019 |
| Předmět: |
Physics
Binary number FOS: Physical sciences Astronomy and Astrophysics 01 natural sciences Combinatorics Secondary component Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science 0103 physical sciences Primary component Spectral analysis 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) |
| DOI: | 10.48550/arxiv.1906.01913 |
| Popis: | The early-type massive binary MQ Cen (P$_{orb}$=3.7 d) has been investigated by means of high-resolution ($R\sim48\,000$) spectral analysis and multi-band (Johnson $BVRI$ and Str\"{o}mgren $vby$) light curve modeling. The physical parameters of the components have been found to be $M_1= 4.26\pm0.10$ M$_{\odot}$, $R_1= 3.72\pm0.05 $R$_{\odot}$, $T_{\rm eff1}=16\,600\pm520$ K, and $M_2= 5.14\pm0.09 $M$_{\odot}$, $R_2= 7.32\pm0.03 $R$_{\odot}$, $T_{\rm eff2}=15\,000\pm500$ K for the primary and secondary, respectively. The orbital inclination is $i=87.0\pm0.2$ deg. The distance to MQ Cen has been derived to be $d=2\,460\pm310$ pc which locates it in the Crux OB1 association. However, the age of MQ~Cen ($\sim70$ Myr) is higher than the one reported for the Crux OB1 association ($\sim$6 Myr). The derived masses are implying a spectral type of B5 for the primary and B4 for the secondary component. Nevertheless, the secondary component, which is more massive, appears to be cooler than the primary component: It has completed its lifetime on the main-sequence and it is now positioned at the turn-off point of the giant branch, meanwhile the less massive primary component is still staying on the main-sequence. Comment: 14 pages, 7 figures and 4 tables, accepted for publication in Astrophysics and Space Science |
| Databáze: | OpenAIRE |
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