The complex dynamical past and future of double eclipsing binary CzeV343: Misaligned orbits and period resonance^⋆

¹ Institute of Theoretical Physics, Faculty of Mathematics and Physics, Charles University, V Holešovičkách 2, Praha 8 180 00, Czech Republic
e-mail: pejcha@utf.mff.cuni.cz
² BSObservatory, Modrá 587, 760 01 Zlín, Czech Republic
e-mail: pc@bsobservatory.org
³ Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
⁴ Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
⁵ Núcleo de Astronomía, Universidad Diego Portales, Av. Ejército 441, Santiago, Chile
⁶ Millennium Institute of Astrophysics, Santiago, Chile
⁷ Hvězdárna Jaroslava Trnky ve Slaném, Nosačická 1713, Slaný 1 274 01, Czech Republic
⁸ Variable Star and Exoplanet Section, Czech Astronomical Society, Fričova 298, 251 65 Ondřejov, Czech Republic

Received: 23 June 2022
Accepted: 11 August 2022

Abstract

CzeV343 (=V849 Aur) was previously identified as a candidate double eclipsing binary (2+2 quadruple), where the orbital periods of the two eclipsing binaries (P_A ≈ 1.2 days and P_B ≈ 0.8 days) lie very close to a 3:2 resonance. Here, we analyze 11 yr of ground-based photometry, four sectors of Transiting Exoplanet Survey Satellite (TESS) 2-min and full-frame photometry, and two optical spectra. We construct a global model of our photometry, including apsidal motion of binary A and the light-travel time effect (LTTE) of the mutual outer orbit, and explore the parameter space with Markov chain Monte Carlo. We estimate component masses for binary A (1.8 + 1.3 M_⊙) and binary B (1.4 + 1.2 M_⊙). We identify the pseudo-synchronous rotation signal of binary A in TESS photometry. We detect apsidal motion in binary A with a period of about 33 yr, which is fully explained by tidal and rotational contributions of stars aligned with the orbit. The mutual orbit has a period of about 1450 days and an eccentricity of about 0.7. The LTTE amplitude is small, which points to low inclination of the outer orbit and a high degree of misalignment with the inner orbits. We find that when apsidal motion and the mutual orbit are taken into account, the orbital period resonance is exact to within 10⁻⁵ cycles/day. Many properties of CzeV343 are not compatible with requirements of the 3:2 resonance capture theory for coplanar orbits. Future evolution of CzeV343 can lead to mergers, triple common envelope, double white dwarf binaries, or a Type Ia supernova. More complex evolutionary pathways will likely arise from dynamical instability caused by orbital expansion when either of the binaries undergoes mass transfer. This instability has not been explored so far in 2+2 quadruples.