Three Nearby K-Giants with Planets: Accurate Determination of Basic Parameters, Including an Analysis of Metallicity Based on Fe I Lines
- 2 Downloads
Fundamental parameters, including the effective temperature Teff, surface gravity logg, mass M, luminosity L, radius R, and age t, are determined for three bright, nearby K-giants, β Gem (K0 III), μ Leo (K2 III), and α Tau (K5 III), It is notable that around all three stars the giant planets have been found. Our results are compared with published high-precision data for benchmark stars included in the Gaia project. Very good agreement was obtained for all three giants with these data for the basic parameters Teff, logg, and M, although our technique of their determination was simpler. Special attention was devoted to analysis of the Fe I lines which are the basis of a simultaneous determination of the metallicity index [Fe/H] and microturbulent parameter Vt. The equivalent widths W of the Fe I lines are automatically measured from published spectra for the benchmark stars. An analysis of Fe I lines from the list of “golden lines” selected in a study of benchmark stars led to the conclusion that the excitation potential El of the low level of the lines plays an substantial role in determining [Fe/H] and Vt. It is shown that in the case of the early K-giants β Gem and μ Leo with temperatures Teff between 4400 and 4900 K for lines in the range of W from 100 to 300 mÅ there is a dependence of the [Fe/H] and Vt values on El. This dependence was not taken into account earlier is studies of the K-giants, in particular in the Fe I lines analysis of the benchmark stars. It is shown that a correct accounting for it leads an ambiguity in the determination of [Fe/H] and Vt for β Gem and μ Leo. In the case of the coolest K-giant α Tau (Aldebaran) with a temperature Teff = 3920K, this effect seems to be less pronounced. Recommendations are given for the Fe I lines selection for [Fe/H] and Vt determination. It is sonfirmed for the example of the three stars studied here that the non-LTE effects in the Fe I lines for the K-giants with normal metallicity are very minor, so they cannot be the reason of the revealed ambiguity in [Fe/H] and Vt. values. The low ratios of the carbon 12C/13C and oxygen 16O/17O isotopes confirm that all three giants passed the phase of deep convective mixing.
Keywordsred giants basic parameters
Unable to display preview. Download preview PDF.
- 4.A. V. Popkov and S. B. Popov, Izv.Krym.Astrofiz.Obs.114, 70 (2018).Google Scholar
- 10.F. van Leeuwen, Hipparcos, the New Reduction of the Raw Data., Springer, Dordrecht (2007).Google Scholar
- 15.I. Ramírez andC. A. Prieto, Astrophys. J.743, 135 (2011).Google Scholar
- 16.R. E. Luck, Astron. J. 150, 88 (2015).Google Scholar
- 28.W. Kang and S.-G. Lee, Mon. Not. Roy. Astron. Soc. 425, 3162 (2012).Google Scholar
- 29.L. I. Mashonkina, T. M. Sitnova, and Yu. V. Pakhomov,Pis’ma v Astron. zh. 42, 667 (2016).Google Scholar
- 30.T. Ryabchikova, N. Piskunov, R. L. Kurucz, et al., Physica Scripta 90, 054005 (2015).Google Scholar
- 32.R. Kurucz, Mem. Soc. Astron. Italiana 75, 1 (2004).Google Scholar
- 38.L. S. Lyubimkov, Astrophysics 59, 472 (2016).Google Scholar