Photometric and Spectroscopic Observations of Exoplanet Transit Events - Planetary Exploration and Science: Recent Results and Advances - page 280

HAT-P-10b

HAT-P-19b

-0.80 0.10

0.12

-0.78

0.14

-0.76

Observation
Model

0.16

Observation
Model

-0.74

56270.05 56270.10 56270.15 56270.20

56270.95 56271.00 56271.05 56271.10

BJD (2400000+)

BJD (2400000+)

1.14

WASP-43b

1.16

1.18

1.20

1.22

observation
Model

1.24

56250.36 56250.38 56250.40 56250.42 56250.44

BJD (2400000+)

Fig. 11.5 The light curves of the observational transits and fitted models of the exoplanet systems
HAT-P-10b/WASP-11b, HAT-P-19b, and WASP-43b

11.5 Conclusions

The results from the analysis of our new data can be summarized as follows:

1. Using the JKTEBOP code, we analyzed new observational light curves of HAT-
P-10b/ WASP-11b, HAT-P-19b, and WASP-43b. The fractional radii (ra C rb),
the ratio of the radii, the orbital inclination, the new transit minima, our
transit depth, and transit width were obtained. The new orbital parameters (see
Tab les 11.1 and 11.2 ) of these systems are in agreement with the previous results
(West et al. 2009 ; Bakos et al. 2009 ; Hellier et al. 2011 ; Gillon et al. 2012 ;etc).
2. The timing residuals giving a hint about a period change (see Fig. 11.5 ), which
might be due to the presence of a second planet in the system or the sporadic
asymmetries of transit curves due to star spots on stellar surface result from
magnetic activity (Steffen and Agol 2005 ; Lee et al. 2012 ; etc). More photometric
data are needed to confirm that.