Hostname: page-component-54dcc4c588-b5cpw Total loading time: 0 Render date: 2025-10-09T20:22:22.879Z Has data issue: false hasContentIssue false
  • English
  • Français

T c-trend and terrestrial planet formation: The case of Zeta Reticuli

Published online by Cambridge University Press:  07 March 2018

V. Adibekyano ,
E. Delgado-Mena ,
N. C. Santos ,
S. G. Sousa  and
P. Figueira
V. Adibekyano
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal email: Vardan.Adibekyan@astro.up.pt
E. Delgado-Mena
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal email: Vardan.Adibekyan@astro.up.pt
N. C. Santos
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal email: Vardan.Adibekyan@astro.up.pt Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal
S. G. Sousa
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal email: Vardan.Adibekyan@astro.up.pt
P. Figueira
Affiliation:
Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal email: Vardan.Adibekyan@astro.up.pt
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Some studies suggested that the chemical abundance trend with the condensation temperature, T c, is a signature of rocky planet formation. Very recently, a strong T c trend was reported in ζ2 Ret relative to its companion (ζ1 Ret) and was explained by the presence of a debris disk around ζ2 Ret. We re-evaluated the presence and variability of the T c trend in this system with a goal to understand the impact of the presence of the debris disk on a star. Our results confirm the reported abundance difference between ζ2 Ret and ζ1 Ret and its dependence on the T c. However, we also found that the T c trends depend on the individual spectrum used. We conclude that for the ζ Reticuli system, for example, nonphysical factors can be at the root of the T c trends for the case of individual spectra. For more details see Adibekyan et al. (2016b).

Keywords

Planetary systemsstars: abundancesstars: binaries

References

Adibekyan, V., Delgado-Mena, E., Feltzing, S., et al. 2017, AN, 338, 442 Google Scholar
Adibekyan, V., Delgado-Mena, E., Figueira, P., et al. 2016b, A&A, 591, A34 Google Scholar
Adibekyan, V., Delgado-Mena, E., Figueira, P., et al. 2016a, A&A, 592, A87 Google Scholar
Adibekyan, V., Benamati, L., Santos, N. C., et al. 2015, MNRAS, 450, 1900 CrossRefGoogle Scholar
Delgado Mena, E., Tsantaki, M., Adibekyan, V., et al. 2017, [arXiv:1705.04349]Google Scholar
Meléndez, J., Asplund, M., Gustafsson, B., & Yong, D., 2009, ApJ, 704, L66 CrossRefGoogle Scholar
Saffe, C., Flores, M., Jaque Arancibia, M., Buccino, A., & Jofre, E., 2016, A&A, 588, A81 Google Scholar
Sousa, S. G., Santos, N. C., Mortier, A., et al. 2015, A&A, 576, A94 Google Scholar