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The magnetically-active, low-mass, triple system WDS 19312+3607 (Research Note)



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Caballero, J. A. and Montes Gutiérrez, David and Klutsch, A. and Genebriera, J. and Miret, F. X. and Tobal, T. and Cairol, J. and Pedraz, S. (2010) The magnetically-active, low-mass, triple system WDS 19312+3607 (Research Note). Astronomy & Astrophysics, 520 . ISSN 0004-6361


Official URL: http://dx.doi.org/10.1051/0004-6361/201014419



Aims. We investigated in detail the system WDS 19312+3607, whose primary is an active M4.5Ve star previously inferred to be young (τ ~ 300–500 Ma) based on its high X-ray luminosity. Methods. We collected intermediate- and low-resolution optical spectra taken with 2 m-class telescopes, photometric data from the B to 8 μm bands, and data for eleven astrometric epochs with a time baseline of over 56 years for the two components in the system, G 125–15 and G 125–14. Results. We derived the M4.5V spectral types of both stars, confirmed their common proper motion, estimated their heliocentric distance and projected physical separation, determined their Galactocentric space velocities, and deduced a most-probable age of older than 600 Ma. We discovered that the primary, G 125–15, is an inflated, double-lined, spectroscopic binary with a short period of photometric variability of 1.6 d, which we associated with orbital synchronisation. The observed X-ray and Hα emissions, photometric variability, and abnormal radius and effective temperature of G 125–15 AB are indicative of strong magnetic activity, possibly because of the rapid rotation. In addition, the estimated projected physical separation between G 125–15 AB and G 125–14 of about 1200 AU ensures that WDS 19312+3607 is one of the widest systems with intermediate M-type primaries. Conclusions. G 125–15 AB is a nearby (d ≈ 26 pc), bright (J ≈ 9.6 mag), active spectroscopic binary with a single proper-motion companion of the same spectral type at a wide separation. They are thus ideal targets for specific follow-ups to investigate wide and close multiplicity or stellar expansion and surface cooling because of the lower convective efficiency.

Item Type:Article
Additional Information:

© ESO, 2010.
We thank the anonymous referee for helpful comments and P. G. Pérez González for software help. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofísica de Andalucía. Based on observations made with the Isaac Newton Telescope operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This research made use of the SIMBAD, operated at Centre de Données astronomiques de Strasbourg, France, and NASA's Astrophysics Data System. Financial support was provided by the Universidad Complutense de Madrid, the Comunidad Autónoma de Madrid, and the Spanish Ministerio de Ciencia e Innovación under grants AyA2008-00695, AyA2008-06423-C03-03, and SP2009/ESP-1496.

Uncontrolled Keywords:Binary CM draconis; Digital sky survey; Proper motion; M-dwarfs; Brown dwarfs; Spectroscopic distances; 2mass J05352184-0546085; Evolutionary models; Ultracool dwarfs; Cool neighbors
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
ID Code:37822
Deposited On:23 May 2016 15:13
Last Modified:10 Dec 2018 15:05

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