Study of Eclipsing Binary and Multiple Systems in OB Associations V: MQ Cen in Crux OB1. (arXiv:1906.01913v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bakis_V/0/1/0/all/0/1">V. Bakis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mikulasek_Z/0/1/0/all/0/1">Z. Mikulasek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Janik_J/0/1/0/all/0/1">J. Janik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zejda_M/0/1/0/all/0/1">M. Zejda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tunc_E/0/1/0/all/0/1">E. Tunc</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nitschelm_C/0/1/0/all/0/1">C. Nitschelm</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bilir_S/0/1/0/all/0/1">S. Bilir</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liska_J/0/1/0/all/0/1">J. Liska</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bakis_H/0/1/0/all/0/1">H. Bakis</a>
The early-type massive binary MQ Cen (P$_{orb}$=3.7 d) has been investigated
by means of high-resolution ($Rsim48,000$) 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 $M_1= 4.26pm0.10$
M$_{odot}$, $R_1= 3.72pm0.05 $R$_{odot}$, $T_{rm eff1}=16,600pm520$ K,
and $M_2= 5.14pm0.09 $M$_{odot}$, $R_2= 7.32pm0.03 $R$_{odot}$, $T_{rm
eff2}=15,000pm500$ K for the primary and secondary, respectively. The orbital
inclination is $i=87.0pm0.2$ deg. The distance to MQ Cen has been derived to
be $d=2,460pm310$ 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$6 Myr). The derived masses are implying a spectral type
of B5 for the primary and B4 for the secondary component. Nevertheless, the
secondary component, which is more massive, appears to be cooler than the
primary component: It has completed its lifetime on the main-sequence and it is
now positioned at the turn-off point of the giant branch, meanwhile the less
massive primary component is still staying on the main-sequence.
The early-type massive binary MQ Cen (P$_{orb}$=3.7 d) has been investigated
by means of high-resolution ($Rsim48,000$) 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 $M_1= 4.26pm0.10$
M$_{odot}$, $R_1= 3.72pm0.05 $R$_{odot}$, $T_{rm eff1}=16,600pm520$ K,
and $M_2= 5.14pm0.09 $M$_{odot}$, $R_2= 7.32pm0.03 $R$_{odot}$, $T_{rm
eff2}=15,000pm500$ K for the primary and secondary, respectively. The orbital
inclination is $i=87.0pm0.2$ deg. The distance to MQ Cen has been derived to
be $d=2,460pm310$ 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.
http://arxiv.org/icons/sfx.gif
