Searching for condensation temperature trends in HD 133131

MIQUELARENA, P.; ALACORIA, J.; SAFFE, C

Tucumán

Congreso; IV Jornadas de Astrofísica Estelar; 2022

The search of chemical signature of planet formation is possible due to the achieved high precision in stellar parameters and chemical abundances derived last years (e.g. Meléndez et al. 2009, Mack et al. 2016, Saffe et al. 2019). Is believed that binary systems are propitious laboratories to study this chemical signatures, specially when they have physically similar components. HD 133131 is a twin binary (G2V+G2V), where HD 133131A has two planets of 1.31 Mj and 0.63 Mj orbiting at 1.44 au and 4.79 au respectively, and HD 133131B has a planet of 2.5 Mj orbiting at 6.4 au (Teske et al. 2016). The previous abundance analysisshowed a depletion of refractory elements in HD 133131A, that could also be interpreted as an accretion of refractory material in HD 133131B. Different scenarios are proposed to explain this results, including de planetary formation. In this work we derived both stellar parameters and high-precision chemical abundances of this system taking advantage of the non-solar-scaled method (Saffe et al. 2018), in an effort to improve the precision of the previous results.