Secular changes in the orbits of the quadruple system VW LMi
Abstract
VW~LMi is the tightest known quadruple system with 2+2 hierarchy. It consists of a W UMa-type eclipsing binary (P12 = 0.47755 days) and another detached non-eclipsing binary (P34 = 7.93 days) orbiting around a common center of mass is about P1234 = 355 days. We present new observations of the system extending the time baseline to study long-term perturbations in the system and to improve orbital elements. The multi-dataset modeling of the system (4 radial-velocity curves for the components and the timing data) clearly showed an apsidal motion in the non-eclipsing binary at a rate of 4.6 degrees/yr, but no other perturbations. This is consistent with the nearly co-planarity of the outer, 355-day orbit, and the 7.93-day orbit of the non-eclipsing binary. Extensive N-body simulations enabled us to constrain the mutual inclination of the non-eclipsing binary and the outer orbits to j34-1234 < 10 degrees.
Keywords
Cite
@article{arxiv.2003.08169,
title = {Secular changes in the orbits of the quadruple system VW LMi},
author = {T. Pribulla and E. Puha and T. Borkovits and J. Budaj and Z. Garai and E. Guenther and L. Hambalek and R. Komzik and E. Kundra and Gy. M. Szabo and M. Vanko},
journal= {arXiv preprint arXiv:2003.08169},
year = {2020}
}
Comments
12 pages, 7 figures, MNRAS in press