The quadruple system HIP 45734
arXiv:2001.08798 · doi:10.3847/1538-3881/ab6a13
Abstract
HIP 45734 is a quadruple system of 2+2 architecture located at 68 pc from the Sun. The outer 9" system A,B has a period of ~10^4 yr. The pair Aa,Ab is a visual binary with a period of 20.1 years and an eccentricity of 0.78. Its periastron in 2019.1 was observed spectroscopically, yielding masses (1.10+-0.04 and 0.98+-0.03 M_sun) and orbital parallax, 14.90+-0.37 mas. The masses, luminosities, and colors approximately agree with evolutionary models of main sequence stars. The component Aa has a detectable lithium line, whereas in Ab it is absent. The pair Ba,Bb is a single-lined spectroscopic binary with a period of 0.55552 day and an orbital inclination of ~45 deg derived by modeling the rotationally broadened line profile with ``flat bottom''. The mass of Bb is ~0.4 M_sun. The star B is chromospherically active (an x-ray source); its flux is modulated with the orbital period by starspots, in addition to occasional flares. The system is probably older than ~600 Myr; it does not belong to any known moving group.
Accepted by Astronomical Journal; 9 pages, 8 figures, 8 tables
References in corpus (8)
- Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties
- The Dartmouth Stellar Evolution Database
- Search for Associations Containing Young stars (SACY): I. Sample & Searching Method
- The Hipparcos-Gaia Catalog of Accelerations
- Ten years of speckle interferometry at SOAR
- Speckle interferometry at SOAR in 2018
- SPOTS: The Search for Planets Orbiting Two Stars. III. Complete Sample and Statistical Analysis
- Wolf 1130: A Nearby Triple System Containing a Cool, Ultramassive White Dwarf