TYC 3340-2437-1: A Quadruple System with A Massive Star
Abstract
Hierarchical massive quadruple systems are ideal laboratories for examining the theories of star formation, dynamical evolution, and stellar evolution. The successive mergers of hierarchical quadruple systems might explain the mass gap between neutron stars and black holes. Looking for light curves of O-type binaries identified by LAMOST, we find a (2+2) quadruple system: TYC 3340-2437-1, located in the stellar bow-shock nebula (SBN). It has a probability of over 99.99\% being a quadruple system derived from the surface density of the vicinity stars. Its inner orbital periods are 3.390602(89) days and 2.4378(16) days, respectively, and the total mass is about (11.47 + 5.79) + (5.2 + 2.02) = 24.48 . The line-of-sight inclinations of the inner binaries, B and B, are 55.94 and 78.2 degrees, respectively, indicating that they are not co-planar. Based on observations spanning 34 months and the significance of the astrometric excess noise () in Gaia DR3 data, we guess that its outer orbital period might be a few years. If it were true, the quadruple system might form through the disk fragmentation mechanism with outer eccentric greater than zero. This eccentricity could be the cause of both the arc-like feature of the SBN and the noncoplanarity of the inner orbit. The outer orbital period and outer eccentric could be determined with the release of future epoch astrometric data of Gaia.
Cite
@article{arxiv.2403.12771,
title = {TYC 3340-2437-1: A Quadruple System with A Massive Star},
author = {Jiao Li and Chao Liu and Changqing Luo and Bo Zhang and Jiang-Dan Li and Jia-Dong Li and Zhan-Wen Han and Xue-Fei Chen and Lu-Qian Wang and Min Fang and Li-Feng Xing and Xi-Liang Zhang and Chichuan Jin},
journal= {arXiv preprint arXiv:2403.12771},
year = {2024}
}