Photometric and Spectroscopic Observations of Exoplanet Transit Events - Planetary Exploration and Science: Recent Results and Advances - page 279

Table 11.2 The result about the transit and orbital parameters of HAT-P-10b/WASP-11b, HAT-P-
19b, and WASP-43b
Parameters HAT-P-10b/WASP-11b HAT-P-19b WASP-43b

rA C rb 0.088 ˙ 0.002 0.087 ˙ 0.003

K(Drb/rA) 0.130 ˙ 0.002 0.141 ˙ 0.002

Orbital inclination
i(deg)

89.931 ˙ 8.52 89.836 ˙ 4.59

Our transit minima
(BJD)

2456,271.01479 ˙ 2456,270.1160 ˙ 2,456,250.4201 ˙

0.00009 0.0003 0.0007

Our transit depth
(mag)

0.0229 ˙ 0.0004 0.0251 ˙ 0.0006 0.026 ˙ 0.003

Our transit width
(minute)

146.9 ˙ 1 162.3 ˙ 2 69.5 (fixed)

RMS of residuals
(mmag)

3.733 3.029

The orbital
ephemeris (BJD)

2454,729.9071(2) C 2,455,091.5354(2) C 2,455,528.8685(1) C

3.7224810(9) 4.0087788(1) 0.81347438(2)

reason is that these quantities are only very weakly correlated for a wide variety of
the light curve shapes, which is better than solution convergence. We only analyzed
the data of HAT-P-10b/WASP-11b, HAT-P-19b, and WASP-43b. After a lot runs,
we obtained the fractional radii (ra C rb), the ratio of the radii, orbital inclination,
new transit minima, our transit depth, and transit width. Our new transit orbital
parameters are listed in Table 11.2 . The errors of the parameters on the light curves
used the Monte Carlo simulation algorithm (Southworth et al. 2004 , 2005 ). These
methods could give us more reliable results (Fig. 11.6 ).

11.4.2 The Period Analysis

We also collected minima times from ETD (Poddany et al. 2010 ), AXA (Amateur
Exoplanet Archive) and other published papers. The timings were transformed from
HJD into BJD using the online applets2 developed by Eastman et al. ( 2010 ). Using
a linear least square fit, new linear ephemeris was obtained in Table 11.2 and O-C
diagrams are displayed in Fig. 11.5 . The points represent the O-C data (The solid
points represent our new data), and the solid lines represent polynomial fits. As
can be seen from Fig. 11.5 , it seems that the period variation shows polynomial
curves.