A compositional link between rocky exoplanets and their host stars

• Type: Article in International Scientific Journal
• Date: 2021

Authors

Adibekyan, V (Author) Other; Dorn, C (Author) Other; Sousa, SG (Author) FCUP; N.C. Santos (Author) FCUP; Bitsch, B (Author) Other; Israelian, G (Author) Other; Mordasini, C (Author) Other; Barros, SCC (Author) FCUP; Mena, ED (Author) FCUP; Demangeon, ODS (Author) Other; Faria, JP (Author) Other; Figueira, P (Author) Other; Hakobyan, AA (Author) Other; Oshagh, M (Author) Other; Soares, BMTB (Author) Other; Kunitomo, M (Author) Other; Takeda, Y (Author) Other; Jofre, E (Author) Other; Petrucci, R (Author) Other; Martioli, E (Author) Other

Journal

Title: Science

Vol. 374

Pages: 330-+

ISSN: 0036-8075

Publisher: American Association for the Advancement of Science

Indexing

ISI Web of Knowledge - 67 Citations

Scopus - 69 Citations

Other information

Authenticus ID: P-00V-MBP

DOI: 10.1126/science.abg8794

Abstract (EN): Stars and planets both form by accreting material from a surrounding disk. Because they grow from the same material, theory predicts that there should be a relationship between their compositions. In this study, we search for a compositional link between rocky exoplanets and their host stars. We estimate the iron-mass fraction of rocky exoplanets from their masses and radii and compare it with the compositions of their host stars, which we assume reflect the compositions of the protoplanetary disks. We find a correlation (but not a 1:1 relationship) between these two quantities, with a slope of >4, which we interpret as being attributable to planet formation processes. Super-Earths and super-Mercuries appear to be distinct populations with differing compositions, implying differences in their formation processes.

Language: English

Type (Professor's evaluation): Scientific

No. of pages: 34