Photometric and Spectroscopic Observations of Exoplanet Transit Events - Planetary Exploration and Science: Recent Results and Advances - page 277

0.09

HAT-P-10b

20121209 HAT-P-19b

-0.80 20121208

0.10

0.11

-0.78

0.12

0.13

-0.76

0.14

0.15

-0.74

0.16

0.17

56270.90 56270.95 56271.00 56271.05 56271.10

56270.05 56270.10 56270.15 56270.20

BJD (2400000+)

BJD (2400000+)

1.14

0.04

WASP-43b 20121118

20121207

HAT-P-25

1.16

0.06

1.18

0.08

1.20

0.10

1.22

0.12

1.24

56268.95 56269.00 56269.05 56269.10 56269.15 56269.20

56250.34 56250.36 56250.38 56250.40 56250.42 56250.44

HJD(24,00000+)

BJD (2400000+)

0.60

20121209

-0.62 HAT-P-20b

WASP36 20121117

0.62

-0.60

0.64

-0.58

0.66

-0.56

0.68

B

0.70

-0.54

0.26 0.28 0.30 0.32 0.34 0.36 0.38 0.40 0.42 0.44

0.24 0.26 0.28 0.30 0.32 0.34 0.36 0.38

HJD (2456249)

HJD(2456271+)

Fig. 11.4 New light curves of the observed transits (HAT-P-10b/ WASP-11b, HAT-P-19b, WASP-
43b, WASP-36b, HAT-P-25b, and HAT-P-20b) using the 85-cm telescope at Xinglong Station,
NAOC

11.4 Results and Analysis

11.4.1 Light Curve Analysis

Our transit curves are modeled using JKTEBOP code (Southworth 2008 , 2009 )and
adopting quadratic limb-darkening law (Claret 2000 ). The JKTEBOP fits for the
sum of fractional radii (ra C rb) and ratio of the radii (Southworth et al. 2005 ). The