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

We explore the effects of an undetected outer giant planet on the dynamics,observability, and stability of Systems with Tightly-packed Inner Planets(STIPs). We use direct numerical simulations along with secular theory andsynthetic secular frequency spectra to analyze how analogues of Kepler-11 andKepler-90 behave in the presence of a nearly co-planar, Jupiter-like outerperturber with semi-major axes between 1 and 5.2 au. Most locations of theouter perturber do not affect the evolution of the inner planetary systems,apart from altering precession frequencies. However, there are locations atwhich an outer planet causes system instability due to, in part, seculareccentricity resonances. In Kepler-90, there is a range of orbital distancesfor which the outer perturber drives planets b and c, through secularinteractions, onto orbits with inclinations that are $\sim16^\circ$ away fromthe rest of the planets. Kepler-90 is stable in this configuration. Suchsecular resonances can thus affect the observed multiplicity of transitingsystems. We also compare the synthetic apsidal and nodal precession frequencieswith the secular theory and find some misalignment between principalfrequencies, indicative of strong interactions between the planets (consistentwith the system showing TTVs). First-order libration angles are calculated toidentify MMRs in the systems, for which two near-MMRs are shown in Kepler-90,with a 5:4 between b and c, as well as a 3:2 between g and h.

The Dynamics of Tightly-packed Planetary Systems in the Presence of an Outer Planet: case studies using Kepler-11 and Kepler-90