The impact of tidal friction evolution on the orbital decay of ultra-short period planets
| Autor: | Lee R. Spitler, Jorge I. Zuluaga, Carolina García-Carmona, Christian Schwab, Mario Sucerquia, Jaime A. Alvarado-Montes |
|---|---|
| Rok vydání: | 2021 |
| Předmět: |
Earth and Planetary Astrophysics (astro-ph.EP)
Physics Angular momentum 010308 nuclear & particles physics FOS: Physical sciences Astronomy and Astrophysics Astrophysics Dissipation Orbital decay 01 natural sciences Exoplanet Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Planet Stellar mass loss 0103 physical sciences Dissipative system Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Tidal acceleration 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics Astrophysics - Earth and Planetary Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. |
| ISSN: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stab1081 |
| Popis: | Unveiling the fate of ultra-short period (USP) planets may help us understand the qualitative agreement between tidal theory and the observed exoplanet distribution. Nevertheless, due to the time-varying interchange of spin-orbit angular momentum in star-planet systems, the expected amount of tidal friction is unknown and depends on the dissipative properties of stellar and planetary interiors. In this work, we couple structural changes in the star and the planet resulting from the energy released per tidal cycle and simulate the orbital evolution of USP planets and the spin-up produced on their host star. For the first time, we allow the strength of magnetic braking to vary within a model that includes photo-evaporation, drag caused by the stellar wind, stellar mass loss, and stellar wind enhancement due to the in-falling USP planet. We apply our model to the two exoplanets with the shortest periods known to date, NGTS-10b and WASP-19b. We predict they will undergo orbital decay in time-scales that depend on the evolution of the tidal dissipation reservoir inside the star, as well as the contribution of the stellar convective envelope to the transfer of angular momentum. Contrary to previous work, which predicted mid-transit time shifts of $\sim30-190$ s over 10 years, we found that such changes would be smaller than 10 s. We note this is sensitive to the assumptions about the dissipative properties of the system. Our results have important implications for the search for observational evidence of orbital decay in USP planets, using present and future observational campaigns. Accepted for publication in MNRAS. 13 pages, 10 figures |
| Databáze: | OpenAIRE |
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