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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We characterize the radii and masses of the star and planets in the Kepler-59system, as well as their orbital parameters. The star parameters are determinedthrough a standard spectroscopic analysis, resulting in a mass of $1.359\pm0.155\,M_\odot$ and a radius of $1.367\pm 0.078\,R_\odot$. The planetary radiiobtained are $1.5\pm 0.1\,R_\oplus$ for the inner and $2.2\pm 0.1\,R_\oplus$for the outer planet. The orbital parameters and the planetary masses aredetermined by the inversion of Transit Timing Variations (TTV) signals. Forthis, we consider two different data sets, one provided by Holczer et al. 2016,with TTVs only for the planet Kepler-59c, and the other provided by Rowe et al.2015, with TTVs signals for both planets. The inversion method is carried outby applying an algorithm of Bayesian inference (MultiNest) combined with anefficient N-body integrator (Swift). For each of the data sets, two possiblesolutions are found, both having the same probability according to theircorresponding Bayesian evidences. All four solutions appear to beindistinguishable within their 2-$\sigma$ uncertainties. Nevertheless,statistical analyses show that the solutions from Rowe et al. 2015 data bettercharacterize the data. The first and second solutions identify masses of$5_{-2}^{+4}~M_{\mathrm{\oplus}}$ and $4.6_{-2.0}^{+3.6}~M_{\mathrm{\oplus}}$,and $3.0^{+0.8}_{-0.8}~M_{\mathrm{\oplus}}$ and$2.6^{+1.9}_{-0.8}~M_{\mathrm{\oplus}}$ for the inner and outer planet,respectively. This points to a system with an inner super-Earth and an outermini-Neptune. Dynamical studies show the planets have almost co-planar orbitswith small eccentricities ($e<0.1$), close but not into the 3:2 mean motionresonance. Stability analysis indicates that this configuration is stable overmillion years of evolution.

A super-Earth and a mini-Neptune around Kepler-59