Analysis of eclipsing binaries in multiple stellar systems: the case of V1200 Centauri

Abstract

We present a new analysis of the multiple star V1200 Centauri based on the most recent observations for this system. We used the photometric observations from the Solaris network and the TESS telescope, combined with the new radial velocities from the CHIRON spectrograph and those published in the literature. We confirmed that V1200 Cen consists of a 2.5-day eclipsing binary orbited by a third body. We derived the parameters of the eclipsing components, which are MAa = 1.393 ± 0.018 M⊙, RAa = 1.407 ± 0.014 R⊙ and Teff, Aa = 6 588 ± 58 K for the primary, and MAb = 0.863 3 ± 0.008 1 M⊙, RAb = 1.154 ± 0.014 R⊙ and Teff, Ab = 4 475 ± 68 K for the secondary. Regarding the third body, we obtained significantly different results than previously published. The period of the outer orbit is found to be 180.4 days, implying a minimum mass MB = 0.871 ± 0.020 M⊙. Thus, we argue that V1200 Cen is a quadruple system with a secondary pair composed of two low-mass stars. Finally, we determined the ages of each eclipsing component using two evolution codes, namely MESA and CESTAM. We obtained ages of 16–18.5 Myr and 5.5–7 Myr for the primary and the secondary, respectively. In particular, the secondary appears larger and hotter than predicted at the age of the primary. We concluded that dynamical and tidal interactions occurring in multiples may alter the stellar properties and explain the apparent non-coevality of V1200 Centauri.

BG Ind: the nearest doubly eclipsing, compact hierarchical quadruple system

“…If this assumption was true, IU Aur would be the shortest outer period 2+2 quadruple with Pout = 294 d, but the system needs further investigations. Moreover, note that most recently Marcadon et al (2020) have proposed that the Pout = 180.4 days period outer component of V1200 Cen might also be a binary, forming a more tight half-year-long period quadruple system.…”

Eclipsing Binaries in Dynamically Interacting Close, Multiple Systems

“…It consists of a W UMa-type overcontact EB (P in,A = 0.48 d) and a non-eclipsing second pair with P in,B = 7.93 d. There are also two more compact systems, however, which are currently known as ECHTs, but some authors claim that the third components are actual close binaries. These are IU Aur (P in = 1.83 d; P out = 293.3 d-Drechsel et al [198]; Özdemir et al [156]) and V1200 Cen (P in = 2.48 d; P out = 180.4 d-Marcadon et al [199]).…”

Eclipsing Binaries in Dynamically Interacting Close, Multiple Systems

“…It consists of a W UMatype overcontact EB (P in,A = 0.48 d) and a non-eclipsing second pair with P in,B = 7.93 d. There are also two more compact systems, however, which currently are known as ECHTs, but some authors claim that the third components are actual close binaries. These are IU Aur (P in = 1.83 d; P out = 293.3 d -Drechsel et al [198]; Özdemir et al [157]) and V1200 Cen (P in = 2.48 d; P out = 180.4 d -Marcadon et al [199]).…”