SIMBAD references

2015ApJ...809..107F - Astrophys. J., 809, 107 (2015/August-8)

Multiplicity among F-type stars. II.

FUHRMANN K. and CHINI R.

Abstract (from CDS):

In continuation of our previous study we present an updated census of new companions and model atmosphere analyses for some 50 southern dwarfs, mostly in the mass range 0.90 M 1.10M. For the common-proper-motion companions µ Vir B, HR 2225 B, HD 67199 B, and HD 114853 B, we confirm their physical association from their radial velocities. We report the discovery of the F-type visual binary α For as a field blue straggler and confirm (ζ Ret, HR 5864) or identify (HD 67199, HR 4013, HR 8843) another five mass transfer systems or candidates. For the F stars τ1 Eri and 111 Tau, we present 10σ and 7σ cases for astrometric binaries by virtue of the very accurate van Leeuwen Hipparcos parallaxes. Following the work of Shaya & Olling, we suggest the F-type star ι Vir to be a wide (0.37 pc) hierarchical quadruple system. We confirm the visual binary NLTT 23781/2 as a common-proper-motion object to the very wide (0.54 pc) F star 40 Leo, but discard the G star HD 128987 as an ultra-wide (1.01 pc) physical companion to the α Lib quadruple system on account of a diverse metallicity. The improved statistics of our sample establishes the previously discovered positive correlation of stellar multiplicities with primary mass. For the F star multiplicity census in the mass range 1.10 M 1.70M, we find that at least a quarter consists of triple or higher level systems and at least two out of three F stars are non-single.

Abstract Copyright: © 2015. The American Astronomical Society. All rights reserved.

Journal keyword(s): stars: fundamental parameters - stars: solar-type - stars: statistics - solar neighborhood

Simbad objects: 212

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2015ApJ...809..107F and select 'bookmark this link' or equivalent in the popup menu


2019.09.19-21:50:31

© Université de Strasbourg/CNRS

    • Contact