Transit timing variations, radial velocities and long-term dynamical stability of the system Kepler-410. (arXiv:1901.08485v1 [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:+Pribulla_T/0/1/0/all/0/1">Theodor Pribulla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dupkala_D/0/1/0/all/0/1">Daniel Dupkala</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Subjak_J/0/1/0/all/0/1">Ján Šubjak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Skarka_M/0/1/0/all/0/1">Marek Skarka</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kabath_P/0/1/0/all/0/1">Petr Kabáth</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hambalek_L/0/1/0/all/0/1">Ľubomír Hambálek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Parimucha_S/0/1/0/all/0/1">Štefan Parimucha</a>
Transit timing variations of Kepler-410Ab were already reported in a few
papers. Their semi-amplitude is about 14.5 minutes. In our previous paper, we
found that the transit timing variations could be caused by the presence of a
stellar companion in this system. Our main motivation for this paper was to
investigate variation in a radial-velocity curve generated by this additional
star in the system. We performed spectroscopic observation of Kepler-410 using
three telescopes in Slovakia and Czech Republic. Using the cross-correlation
function, we measured the radial velocities of the star Kepler-410A. We did not
observe any periodic variation in a radial-velocity curve. Therefore, we
rejected our previous hypothesis about additional stellar companion in the
Kepler-410 system. We ran different numerical simulations to study mean-motion
resonances with Kepler-410Ab. Observed transit timing variations could be also
explained by the presence of a small planet near to mean-motion resonance 2:3
with Kepler-410Ab. This resonance is stable on a long-time scale. We also
looked for stable regions in the Kepler-410 system where another planet could
exist for a long time.
Transit timing variations of Kepler-410Ab were already reported in a few
papers. Their semi-amplitude is about 14.5 minutes. In our previous paper, we
found that the transit timing variations could be caused by the presence of a
stellar companion in this system. Our main motivation for this paper was to
investigate variation in a radial-velocity curve generated by this additional
star in the system. We performed spectroscopic observation of Kepler-410 using
three telescopes in Slovakia and Czech Republic. Using the cross-correlation
function, we measured the radial velocities of the star Kepler-410A. We did not
observe any periodic variation in a radial-velocity curve. Therefore, we
rejected our previous hypothesis about additional stellar companion in the
Kepler-410 system. We ran different numerical simulations to study mean-motion
resonances with Kepler-410Ab. Observed transit timing variations could be also
explained by the presence of a small planet near to mean-motion resonance 2:3
with Kepler-410Ab. This resonance is stable on a long-time scale. We also
looked for stable regions in the Kepler-410 system where another planet could
exist for a long time.
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