Dynamical masses of M-dwarf binaries in young moving groups: I - The case of TWA 22 and GJ 2060
Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($<$ 200 Myr) and in the low-mass regime ($\mathrm{<1~M_{\odot}}$). GJ 2060 AB and TWA 22 AB are two rare astrometric M-dwarf binarie...
Gespeichert in:
| Hauptverfasser: | , , |
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| Dokumenttyp: | Article (Journal) Kapitel/Artikel |
| Sprache: | Englisch |
| Veröffentlicht: |
14 Jun 2018
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| In: |
Arxiv
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| Online-Zugang: | Verlag, Volltext: http://arxiv.org/abs/1806.05491
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| Verfasserangaben: | L. Rodet, M. Bonnefoy, S. Durkan, H. Beust, A.-M. Lagrange, J.E. Schlieder, M. Janson, A. Grandjean, G. Chauvin, S. Messina, A.-L. Maire, W. Brandner, J. Girard, P. Delorme, B. Biller, C. Bergfors, S. Lacour, M. Feldt, T. Henning, A. Boccaletti, J.-B. Le Bouquin, J.-P. Berger, J.-L. Monin, S. Udry, S. Peretti, D. Segransan, F. Allard, D. Homeier, A. Vigan, M. Langlois, J. Hagelberg, F. Menard, A. Bazzon, J.-L. Beuzit, A. Delboulbe, S. Desidera, R. Gratton, J. Lannier, R. Ligi, D. Maurel, D. Mesa, M. Meyer, A. Pavlov, J. Ramos, R. Rigal, R. Roelfsema, G. Salter, M. Samland, T. Schmidt, E. Stadler, and L. Weber |
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| 245 | 1 | 0 | |a Dynamical masses of M-dwarf binaries in young moving groups |b I - The case of TWA 22 and GJ 2060 |c L. Rodet, M. Bonnefoy, S. Durkan, H. Beust, A.-M. Lagrange, J.E. Schlieder, M. Janson, A. Grandjean, G. Chauvin, S. Messina, A.-L. Maire, W. Brandner, J. Girard, P. Delorme, B. Biller, C. Bergfors, S. Lacour, M. Feldt, T. Henning, A. Boccaletti, J.-B. Le Bouquin, J.-P. Berger, J.-L. Monin, S. Udry, S. Peretti, D. Segransan, F. Allard, D. Homeier, A. Vigan, M. Langlois, J. Hagelberg, F. Menard, A. Bazzon, J.-L. Beuzit, A. Delboulbe, S. Desidera, R. Gratton, J. Lannier, R. Ligi, D. Maurel, D. Mesa, M. Meyer, A. Pavlov, J. Ramos, R. Rigal, R. Roelfsema, G. Salter, M. Samland, T. Schmidt, E. Stadler, and L. Weber |
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| 520 | |a Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages ($<$ 200 Myr) and in the low-mass regime ($\mathrm{<1~M_{\odot}}$). GJ 2060 AB and TWA 22 AB are two rare astrometric M-dwarf binaries respectively members of the AB Doradus and Beta Pictoris moving groups. As their dynamical mass can be measured within a few years, they can be used to calibrate the evolutionary tracks and set new constraints on the age of young moving groups. We find a total mass of $\mathrm{0.18\pm 0.02~M_\odot}$ for TWA 22. That mass is in good agreement with model predictions at the age of the Beta Pic moving group. We obtain a total mass of $\mathrm{1.09 \pm 0.10~M_{\odot}}$ for GJ 2060. We estimate a spectral type of M$1\pm0.5$, $\mathrm{L/L_{\odot}=-1.20\pm0.05}$ dex, and $\mathrm{T_{eff}=3700\pm100}$ K for GJ 2060 A. The B component is a M$3\pm0.5$ dwarf with $\mathrm{L/L_{\odot}=-1.63\pm0.05}$ dex and $\mathrm{T_{eff}=3400\pm100}$ K. The dynamical mass of GJ 2060 AB is inconsistent with the most recent models predictions (BCAH15, PARSEC) for an ABDor age in the range 50-150 Myr. It is 10 to 20\% (1-2 sigma, depending on the assumed age) above the models predictions, corresponding to an underestimation of $0.10$ to $0.20~\mathrm{M_\odot}$. Coevality suggests a young age for the system ($\sim$ 50 Myr) according to most evolutionary models. TWA 22 validates the predictions of recent evolutionary tracks at $\sim$20 Myr. On the other hand, we evidence a 1-2 sigma mismatch between the predicted and observed mass of GJ 2060 AB. This slight departure may indicate that one of the star hosts a tight companion. Alternatively, this would confirm the models tendency to underestimate the mass of young low-mass stars. | ||
| 650 | 4 | |a Astrophysics - Solar and Stellar Astrophysics | |
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