The origin of the occurrence rate profile of gas giants inside 100 d
Abstract
We investigate the origin of the period distribution of giant planets. We fit the bias-corrected distribution of gas-giant planets inside 300 d found by Santerne et al. using a planet formation model based on pebble accretion. We investigate two possible initial conditions: a linear distribution of planetary seeds, and seeds injected exclusively on the water and CO icelines. Our simulations exclude the linear initial distribution of seeds with a high degree of confidence. Our bimodal model based on snowlines gives a more reasonable fit to the data, with the discrepancies reducing significantly if we assume the water snowline to be a factor of 3-10 less efficient at producing planets. This model moreover performs better on both the warm/hot Jupiters ratio and a Gaussian mixture model as comparison criteria. Our results hint that the gas-giant exoplanets population inside 300 d is more compatible with planets forming preferentially at special locations.
- Publication:
-
Monthly Notices of the Royal Astronomical Society
- Pub Date:
- August 2017
- DOI:
- 10.1093/mnras/stx1272
- arXiv:
- arXiv:1704.06383
- Bibcode:
- 2017MNRAS.469.5016A
- Keywords:
-
- planets and satellites: formation;
- Astrophysics - Earth and Planetary Astrophysics
- E-Print:
- 8 pages, 6 figures, Accepted for publication in MNRAS. Comments welcome