2019MNRAS.485.4601P -
Mon. Not. R. Astron. Soc., 485, 4601-4616 (2019/June-1)
Two Super-Earths in the 3:2 MMR around KOI-1599.
PANICHI F., MIGASZEWSKI C. and GOZDZIEWSKI K.
Abstract (from CDS):
We validate the planetary origin of the KOI-1599 transit time variations (TTVs) with statistical and dynamical tests. We re-analysed KEPLER Q1-Q17 light-curves of the star, and we independently derived the TTVs. They appear as strongly anticorrelated, suggestive of two mutually interacting planets. We found similar radii of the candidates, 1.9 ± 0.2R⊕ for the inner KOI-1599.02, and 1.9 ± 0.3R⊕ for the outer KOI-1599.01. The standard MCMC TTV analysis constrains the planet masses safely below the dynamical instability limit of ≃3 MJup. The best-fitting MCMC model yields (9.0±0.3) M⊕, and (4.6±0.3) M⊕, for the inner and the outer planet, respectively. The planets are trapped in 3:2 mean motion resonance (MMR) with anti-aligned apsides (Δp = 180°) at low-eccentric (e ≃ 0.01) orbits. However, we found that the TTV mass determination depends on eccentricity priors with the dispersion in the (0.01,0.05) range. They permit a second family of TTV models with smaller masses of ≃7 M⊕, and ≃3.6 M⊕, respectively, exhibiting two modes of Δp = 0°, 180° librations. The 3:2 MMR is dynamically robust and persists for both modes. In order to resolve the mass duality, we re-analysed the TTV data with a quasi-analytic model of resonant TTV signals. This model favours the smaller masses. We also reproduced this model by simulating the migration capture of the system into the 3:2 MMR.
Abstract Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Journal keyword(s):
celestial mechanics - planetary systems - stars: individual: KOI-1599
Status at CDS
:
Large table(s) will be appraised for possible ingestion in VizieR.
Simbad objects:
6
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