English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Observations of hot Jupiter type exoplanets suggest that their orbital perioddistribution depends on the metallicity of their host star. We investigate herewhether the impact of the stellar metallicity on the evolution of the tidaldissipation inside the convective envelope of rotating stars and its resultingeffect on the planetary migration might be a possible explanation for thisobserved statistical trend.  We use a frequency-averaged tidal dissipation formalism coupled to an orbitalevolution code and to rotating stellar evolution models to estimate the effectof a change of stellar metallicity on the evolution of close-in planets. Weconsider here two different stellar masses: 0.4 and 1.0 $M_{\odot}$ evolvingfrom the early pre-main sequence phase up to the red giant branch.  We show that the metallicity of a star has a strong effect on the stellarparameters which in turn strongly influence the tidal dissipation in theconvective region. While on the pre-main sequence the dissipation of a metalpoor Sun-like star is higher than the dissipation of a metal rich Sun-likestar, on the main sequence it is the opposite. However, for the $0.4~M_{\odot}$star, the dependence of the dissipation with metallicity is much less visible.  Using an orbital evolution model, we show that changing the metallicity leadsto different orbital evolutions (e.g., planets migrate farther out from aninitially fast rotating metal rich star). By using this model, we qualitativelyreproduced the observational trends of the population of hot Jupiters with themetallicity of their host stars. However, more steps are needed to improve ourmodel to try to quantitatively fit our results to the observations. Namely, weneed to improve the treatment of the rotation evolution in the orbitalevolution model and ultimately we need to consistently couple of the orbitalmodel to the stellar evolution model.

astronomy and astrophysics

Tidal dissipation in rotating low-mass stars and implications for the  orbital evolution of close-in massive planets. II. Effect of stellar  metallicity