WASP-92, WASP-93 and WASP-118: Transit timing variations and long-term stability of the systems. (arXiv:1903.02804v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gajdos_P/0/1/0/all/0/1">Pavol Gajdoš</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanko_M/0/1/0/all/0/1">Martin Vaňko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evans_P/0/1/0/all/0/1">Phil Evans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bretton_M/0/1/0/all/0/1">Marc Bretton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molina_D/0/1/0/all/0/1">David Molina</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferratfiat_S/0/1/0/all/0/1">Stéphane Ferratfiat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Girardin_E/0/1/0/all/0/1">Eric Girardin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gu%7B%5Cdh%7Dmundsson_S/0/1/0/all/0/1">Snævarr Guðmundsson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scaggiante_F/0/1/0/all/0/1">Francesco Scaggiante</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parimucha_S/0/1/0/all/0/1">Štefan Parimucha</a>
We studied three exoplanetary systems with transiting planets: WASP-92,
WASP-93 and WASP-118. Using ground-based photometric observations of WASP-92
and WASP-93 and textit{Kepler-K2} observations of WASP-118, we redetermined
the orbital and physical parameters of these planets. The precise times of all
transits were determined. We constructed O-C diagrams of transits and analysed
possible transit timing variations. We did not observe any significant
deviation from a linear ephemeris for any of the selected exoplanets. We put
upper-mass limits for other hypothetical planets in these systems. Using
long-term numerical simulation, we looked for stable regions where another
planet could exist for a long time. We used the maximum eccentricity method for
this purpose. We discuss the influence of values of initial inclination and
eccentricity on the shape and size of regions of stability.
We studied three exoplanetary systems with transiting planets: WASP-92,
WASP-93 and WASP-118. Using ground-based photometric observations of WASP-92
and WASP-93 and textit{Kepler-K2} observations of WASP-118, we redetermined
the orbital and physical parameters of these planets. The precise times of all
transits were determined. We constructed O-C diagrams of transits and analysed
possible transit timing variations. We did not observe any significant
deviation from a linear ephemeris for any of the selected exoplanets. We put
upper-mass limits for other hypothetical planets in these systems. Using
long-term numerical simulation, we looked for stable regions where another
planet could exist for a long time. We used the maximum eccentricity method for
this purpose. We discuss the influence of values of initial inclination and
eccentricity on the shape and size of regions of stability.
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