Which stars can form planets: Planetesimal formation at low metallicities
| dc.contributor.author | Andama, Geoffrey | |
| dc.contributor.author | Mah, Jingyi | |
| dc.contributor.author | Bitsch, Bertram | |
| dc.date.accessioned | 2024-03-15T09:51:39Z | |
| dc.date.available | 2024-03-15T09:51:39Z | |
| dc.date.issued | 2024-01-26 | |
| dc.description.abstract | The diversity of exoplanets has been linked to the disc environment in which they form, where the host star metallicity and the formation pathways play a crucial role. In the context of the core accretion paradigm, the initial stages of planet formation require the growth of dust material from micrometre-sized to planetesimal-sized bodies before core accretion can kick in. Although numerous studies have been conducted on planetesimal formation, it is still poorly understood how this process takes place in low-metallicity stellar environments. In this work, we explore how planetesimals are formed in stellar environments with primarily low metallicities. We performed global 1D viscous disc evolution simulations, including the growth of dust particles and the evaporation and condensation of chemical species at ice lines. We followed the formation of planetesimals during disc evolution and tested different metallicities, disc sizes, and turbulent viscosity strengths. We find that at solar and sub-solar metallicities, there is a significant increase in the midplane dust-to-gas mass ratios at the ice lines, but this leads to planetesimal formation only at the water–ice line. In our simulations, [Fe/H] = −0.6 is the lower limit of metallicity for planetesimal formation where a few Earth masses of planetesimals can form. Our results further show that for such extreme disc environments, large discs are more conducive than small discs for forming large amounts of planetesimals at a fixed metallicity because the pebble flux can be maintained for a longer time, resulting in a longer and more efficient planetesimal formation phase. At lower metallicities, planetesimal formation is less supported in quiescent discs compared to turbulent discs, which produce larger amounts of planetesimals, because the pebble flux can be maintained for a longer time. The amount of planetesimals formed at sub-solar metallicities in our simulations places a limit on core sizes that could potentially result only in the formation of super-Earths. | en_US |
| dc.identifier.citation | Andama, G., Mah, J., & Bitsch, B. (2024). What stars can form planets: planetesimal formation at low metallicity. Astronomy & Astrophysics, 683(A&A):1-8. https://doi.org/10.1051/0004-6361/202348899 | en_US |
| dc.identifier.issn | 1432-0746 | |
| dc.identifier.uri | https://dir.muni.ac.ug/handle/20.500.12260/622 | |
| dc.language.iso | en | en_US |
| dc.publisher | EDP Sciences | en_US |
| dc.subject | Planets and satellites: formation | en_US |
| dc.subject | Protoplanetary disks | en_US |
| dc.title | Which stars can form planets: Planetesimal formation at low metallicities | en_US |
| dc.type | Article | en_US |