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Imaging and Characterization of Extrasolar Planets with the Next Generation of Space Telescopes

Heavy Metal Rules. I. Exoplanet Incidence and Metallicity

Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal
Geosciences 2019, 9(3), 105;
Received: 28 December 2018 / Revised: 14 February 2019 / Accepted: 20 February 2019 / Published: 27 February 2019
(This article belongs to the Special Issue Detection and Characterization of Extrasolar Planets)
The discovery of only a handful of exoplanets required establishing a correlation between giant planet occurrence and metallicity of their host stars. More than 20 years have already passed from that discovery, however, many questions are still under lively debate: (1) What is the origin of that relation?; (2) What is the exact functional form of the giant planet–metallicity relation (in the metal-poor regime)?; and (3) Does such a relation exist for terrestrial planets? All of these questions are very important for our understanding of the formation and evolution of (exo)planets of different types around different types of stars and are the subject of the present manuscript. Besides making a comprehensive literature review about the role of metallicity on the formation of exoplanets, I also revisited most of the planet–metallicity related correlations reported in the literature using a large and homogeneous data provided by the SWEET-Cat catalog. This study led to several new results and conclusions, two of which I believe deserve to be highlighted in the abstract: (i) the hosts of sub-Jupiter mass planets (∼0.6–0.9 M) are systematically less metallic than the hosts of Jupiter-mass planets. This result might be related to the longer disk lifetime and the higher amount of planet building materials available at high metallicities, which allow a formation of more massive Jupiter-like planets; (ii) contrary to the previous claims, our data and results do not support the existence of a breakpoint planetary mass at 4 M above and below which planet formation channels are different. However, the results also suggest that planets of the same (high) mass can be formed through different channels depending on the (disk) stellar mass i.e., environmental conditions. View Full-Text
Keywords: exoplanets; metallicity; planetary systems; galaxy: solar neighborhood exoplanets; metallicity; planetary systems; galaxy: solar neighborhood
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MDPI and ACS Style

Adibekyan, V. Heavy Metal Rules. I. Exoplanet Incidence and Metallicity. Geosciences 2019, 9, 105.

AMA Style

Adibekyan V. Heavy Metal Rules. I. Exoplanet Incidence and Metallicity. Geosciences. 2019; 9(3):105.

Chicago/Turabian Style

Adibekyan, Vardan. 2019. "Heavy Metal Rules. I. Exoplanet Incidence and Metallicity" Geosciences 9, no. 3: 105.

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