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

Gas giants' early ($\lesssim 5$ Myr) orbital evolution occurs in a disclosing mass in part to photoevaporation driven by high energy irradiance fromthe host star. This process may ultimately overcome viscous accretion todisperse the disc and halt migrating giants by starving their orbits of gas,imprinting on giant planet separations in evolved systems. Inversion of thisdistribution could then give insight into whether stellar FUV, EUV or X-rayflux dominates photoevaporation, constraining planet formation and discevolution models. We use a 1D hydrodynamic code in population syntheses for gasgiants undergoing Type II migration in a viscously evolving disc subject toeither a primarily FUV, EUV or X-ray flux from a pre-solar T Tauri star. Thephotoevaporative mass loss profile's unique peak location and width in eachenergetic regime produces characteristic features in the distribution of giantseparations: a severe dearth of $\lesssim$ 2 M$_{\rm J}$ planets interior to 5AU in the FUV scenario, a sharp concentration of $\lesssim$ 3 M$_{\rm J}$planets between $\approx 1.5 - 2$ AU in the EUV case, and a relative abundanceof $\approx 2 - 3.5$ M$_{\rm J}$ giants interior to 0.5 AU in the X-ray model.These features do not resemble the observational sample of gas giants with massconstraints, though our results do show some weaker qualitative similarities.We thus assess how the differing photoevaporative profiles interact withmigrating giants and address the effects of large model uncertainties as a stepto better connect disc models with trends in the exoplanet population.

The comparative effect of FUV, EUV and X-ray disc photoevaporation on gas giant separations