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Theoretical evolution of Rossby number for solar analog stars

Published online by Cambridge University Press:  07 August 2014

Matthieu Castro ,
Tharcísyo Duarte  and
José Dias do Nascimento Jr.
Matthieu Castro
Affiliation:
Departamento de Física Teórica e Experimental (DFTE), Universidade Federal do Rio Grande do Norte (UFRN), Campus Universitário Lagoa Nova, CEP: 59078-970, Natal (RN), Brazil email: mcastro@dfte.ufrn.br
Tharcísyo Duarte
Affiliation:
Departamento de Física Teórica e Experimental (DFTE), Universidade Federal do Rio Grande do Norte (UFRN), Campus Universitário Lagoa Nova, CEP: 59078-970, Natal (RN), Brazil email: mcastro@dfte.ufrn.br
José Dias do Nascimento Jr.
Affiliation:
Departamento de Física Teórica e Experimental (DFTE), Universidade Federal do Rio Grande do Norte (UFRN), Campus Universitário Lagoa Nova, CEP: 59078-970, Natal (RN), Brazil email: mcastro@dfte.ufrn.br
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Abstract

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Magnetic fields of late-type stars are presumably generated by a dynamo mechanism at the interface layer between the radiative interior and the outer convective zone. The Rossby number, which is related to the dynamo process, shows an observational correlation with activity. It represents the ratio between the rotation period of the star and the local convective turnover time. The former is well determined from observations but the latter is estimated by an empirical iterated function depending on the color index (B-V) and the mixing-length parameter. We computed the theoretical Rossby number of stellar models with the TGEC code, and analyze its evolution with time during the main sequence. We estimated a function for the local convective turnover time corresponding to a mixing-length parameter inferred from a solar model, and compare our results to the estimated Rossby number of 33 solar analogs and twins, observed with the spectropolarimeters ESPaDOnS@CFHT and Narval@LBT.

Keywords

solar analogsmagnetic fieldRossby number
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S302: Magnetic Fields throughout Stellar Evolution , August 2013 , pp. 144 - 145
Copyright
Copyright © International Astronomical Union 2014 

References

do Nascimento, J.-D., da Costa, J. S., & Castro, M. 2013, A&A, 548, L1Google Scholar
Donati, J.-F., Semel, M., Carter, B. D.et al. 1997, MNRAS, 291, 658Google Scholar
Kawaler, S. D. 1988, ApJ, 333, 236Google Scholar
Landin, N. R., Mendes, L. T. S., & Vaz, L. P. R. 2010, A&A, 510, A46Google Scholar
Lovis, C., Dumusque, X., Santos, N. C.et al. 2011, eprint arXiv:1107.5325Google Scholar
Noyes, R. W., Hartmann, S. W., Baliunas, S.et al. 1984, ApJ, 279, 763Google Scholar
Richard, O., Thado, S., & Vauclair, S. 2004, SoPh, 220, 243Google Scholar
Wright, J. T., Marcy, G. W., Paul Butler, R., & Vogt, S. S. 2004, ApJS, 152, 261Google Scholar