This article has an erratum: [https://doi.org/10.1051/0004-6361/201730725e]
Volume 604, August 2017
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||11 August 2017|
The discrepancy between dynamical and theoretical mass in the triplet-system 2MASS J10364483+1521394
1 Department of AstronomyStockholm University, 11418 Stockholm, Sweden
2 Institut für Astro- und Teilchenphysik, Universität Innsbruck, Technikerstr. 25/8, 6020 Innsbruck, Austria
3 Department of Astrophysics, University of Vienna, 1010 Vienna, Austria
4 Astrophysics Research Centre, Queens University, Belfast, BT71 NN, UK
5 Max Planck Institute for Astronomy, 69117 Heidelberg, Germany
6 NASA Goddard Space Flight Center, Greenbelt, MD20771 Maryland, USA
Received: 2 March 2017
Accepted: 5 May 2017
We combine new Lucky Imaging astrometry from New Technology Telescope/AstraLux Sur with already published astrometry from the AstraLux Large M-dwarf Multiplicity Survey to compute orbital elements and individual masses of the 2MASS J10364483+1521394 triple system belonging to the Ursa-Major moving group. The system consists of one primary low-mass M-dwarf orbited by two less massive companions, for which we determine a combined dynamical mass of MB + C = 0.48 ± 0.14 M⊙. We show from the companions’ relative motions that they are of equal mass (with a mass ratio of 1.00 ± 0.03), thus 0.24 ± 0.07 M⊙ individually, with a separation of 3.2 ± 0.3 AU, and we conclude that these masses are significantly higher (30%) than what is predicted by theoretical stellar evolutionary models. The biggest uncertainty remains the distance to the system, here adopted as 20.1 ± 2.0 pc based on trigonometric parallax, whose ambiguity has a major impact on the result. With the new observational data we are able to conclude that the orbital period of the BC pair is 8.41+0.04-0.02yr.
Key words: astrometry / binaries: close / stars: low-mass / stars: kinematics and dynamics
© ESO, 2017
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