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

The Kepler mission has discovered that multiple close-in super-Earth planetsare common around solar-type stars, but their period ratios do not show strongpile-ups near mean motion resonances (MMRs). One scenario is that super-Earthsform in a gas-rich disk, and they interact gravitationally with the surroundinggas, inducing their orbital migration. Disk migration theory predicts, however,that planets would end up at resonant orbits due to their differentialmigration speed. Motivated by the discrepancy between observation and theory,we seek for a mechanism that moves planets out of resonances. We examine theorbital evolution of planet pairs near the magnetospheric cavity during the gasdisk dispersal phase. Our study determines the conditions under which planetscan escape resonances. We perform two-planet N-body simulations, varying theplanet masses, stellar magnetic field strengths, disk accretion rates and gasdisk depletion timescales. As planets migrate outward with the expandingmagnetospheric cavity, their dynamical configurations can be rearranged.Migration of planets is substantial (minor) in a massive (light) disk. When theouter planet is more massive than the inner planet, the period ratio of twoplanets increases through outward migration. On the other hand, when the innerplanet is more massive, the final period ratio tends to remain similar to theinitial one. Larger stellar magnetic field strengths result in planets stoppingtheir migration at longer periods. We highlight \textit{magnetospheric rebound}as an important ingredient able to reconcile disk migration theory withobservations. Even when planets are trapped into MMR during the early gas-richstage, subsequent cavity expansion would induce substantial changes to theirorbits, moving them out of resonance.

Dynamical rearrangement of super-Earths during disk dispersal I. Outline of the magnetospheric rebound model