On the formation of super-Jupiters: Core Accretion or Gravitational Instability?
Fuente:
arXiv
Saved in:
| Main Authors: | , |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866909421287768064 |
|---|---|
| author | Nguyen, M. Adibekyan, V. |
| author_facet | Nguyen, M. Adibekyan, V. |
| contents | The Core Accretion model is widely accepted as the primary mechanism for forming planets up to a few Jupiter masses. However, the formation of super-massive planets remains a subject of debate, as their formation via the Core Accretion model requires super-solar metallicities. Assuming stellar atmospheric abundances reflect the composition of protoplanetary disks, and that disk mass scales linearly with stellar mass, we calculated the total amount of metals in planet-building materials that could contribute to the formation of massive planets. In this work, we studied a sample of 172 Jupiter-mass planets and 93 planets with masses exceeding 4 Mjup. Our results consistently demonstrate that planets with masses above 4 Mjup form in disks with at least as much metal content as those hosting planets with masses between 1 and 4 Mjup, often with slightly higher metallicity, typically exceeding that of the proto-solar disk. We interpret this as strong evidence that the formation of very massive Jupiters is feasible through Core Accretion and encourage planet formation modelers to test our observational conclusions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2412_06594 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | On the formation of super-Jupiters: Core Accretion or Gravitational Instability? Nguyen, M. Adibekyan, V. Earth and Planetary Astrophysics The Core Accretion model is widely accepted as the primary mechanism for forming planets up to a few Jupiter masses. However, the formation of super-massive planets remains a subject of debate, as their formation via the Core Accretion model requires super-solar metallicities. Assuming stellar atmospheric abundances reflect the composition of protoplanetary disks, and that disk mass scales linearly with stellar mass, we calculated the total amount of metals in planet-building materials that could contribute to the formation of massive planets. In this work, we studied a sample of 172 Jupiter-mass planets and 93 planets with masses exceeding 4 Mjup. Our results consistently demonstrate that planets with masses above 4 Mjup form in disks with at least as much metal content as those hosting planets with masses between 1 and 4 Mjup, often with slightly higher metallicity, typically exceeding that of the proto-solar disk. We interpret this as strong evidence that the formation of very massive Jupiters is feasible through Core Accretion and encourage planet formation modelers to test our observational conclusions. |
| title | On the formation of super-Jupiters: Core Accretion or Gravitational Instability? |
| topic | Earth and Planetary Astrophysics |
| url | https://arxiv.org/abs/2412.06594 |