Analysis of HAT-P-16b and TrES-3b Exoplanets by the Transit Timing Variations Method. (arXiv:2109.06108v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Aladag_Y/0/1/0/all/0/1">Y. Alada&#x11f;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Akyuz_A/0/1/0/all/0/1">A. Aky&#xfc;z</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Basturk_O/0/1/0/all/0/1">&#xd6;. Bast&#xfc;rk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aksaker_N/0/1/0/all/0/1">N. Aksaker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Esmer_E/0/1/0/all/0/1">E.M. Esmer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yalcinkaya_S/0/1/0/all/0/1">S. Yal&#xe7;&#x131;nkaya</a>

In this study, the transit observations of HAT-P-16b and TrES-3b exoplanets
were carried out at c{C}”U UZAYMER Observatory with a 50 cm Ritchey Chretien
type telescope. By analyzing the light curves of both exoplanets, system
parameters have been obtained with acceptable models. Some of these parameters
for HAT-P-16 systems were found to be: M$_{P}$=4.172$pm$0.163 M$_{J}$,
R$_{P}$=1.309$pm$0.111 R$_{J}$, a/R$_{*}$=7.1922$pm$0.0017 and
b=0.1003$pm$0.1533 which are consistent with the values given in
cite{2010ApJ…720.1118B}. Also, for the TrES-3 system, the same parameters
were calculated as M$_{P}$=1.959$pm$0.111 M$_{J}$, R$_{P}$=1.320$pm$0.169
R$_{J}$, a/R$_{*}$=6.0656$pm$ 0.4899 and b=0.7892$pm$0.0700. These values are
also consistent with the values given in cite{2007ApJ…663L..37O}. No
significant Transit Timing Variations (TTV) was found as a result of the
Lomb-Scargle (LS) periodogram for HAT-P-16b by using the transit times obtained
from the transit light curves (False Alarm Probabilities — FAP) = %96).
However, a significant periodicity was found at 32.38 days and a secondary
periodicity was found at 41.07 days were determined as a result of the LS
periodogram obtained from the TrES-3b data. We interpret that these periods
with FAP of 3.41 % and 1.88 %, respectively, are close to the rotation period
of the host star. Therefore, these periods could be due to the modulation of
spot-induced light variations.

In this study, the transit observations of HAT-P-16b and TrES-3b exoplanets
were carried out at c{C}”U UZAYMER Observatory with a 50 cm Ritchey Chretien
type telescope. By analyzing the light curves of both exoplanets, system
parameters have been obtained with acceptable models. Some of these parameters
for HAT-P-16 systems were found to be: M$_{P}$=4.172$pm$0.163 M$_{J}$,
R$_{P}$=1.309$pm$0.111 R$_{J}$, a/R$_{*}$=7.1922$pm$0.0017 and
b=0.1003$pm$0.1533 which are consistent with the values given in
cite{2010ApJ…720.1118B}. Also, for the TrES-3 system, the same parameters
were calculated as M$_{P}$=1.959$pm$0.111 M$_{J}$, R$_{P}$=1.320$pm$0.169
R$_{J}$, a/R$_{*}$=6.0656$pm$ 0.4899 and b=0.7892$pm$0.0700. These values are
also consistent with the values given in cite{2007ApJ…663L..37O}. No
significant Transit Timing Variations (TTV) was found as a result of the
Lomb-Scargle (LS) periodogram for HAT-P-16b by using the transit times obtained
from the transit light curves (False Alarm Probabilities — FAP) = %96).
However, a significant periodicity was found at 32.38 days and a secondary
periodicity was found at 41.07 days were determined as a result of the LS
periodogram obtained from the TrES-3b data. We interpret that these periods
with FAP of 3.41 % and 1.88 %, respectively, are close to the rotation period
of the host star. Therefore, these periods could be due to the modulation of
spot-induced light variations.

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