Authors

M. Seeliger, Astrophysical Institute and University Observatory Jena, Schillergaesschen
D. P. Dimitrov, Institute of Astronomy and NAOFollow
D. Kjurkchieva, Shumen University
M. Mallonn, Leibnitz Institut fur Astrophysik Potsdam
M. Fernandez, Instituto de Astrofisica de AndaluciaFollow
M. Kitze, Astrophysical Institute and University Observatory Jena, Schillergaesschen
V. Casanova, Instituto de Astrofisica de Andalucia
G. Maciejewski, N. Copernicus University
J. M. Ohlert, Technische Hochschule Mittelhessen
J. G. Schmidt, Astrophysical Institute and University Observatory Jena, Schillergaesschen
A. Pannicke, Astrophysical Institute and University Observatory Jena, Schillergaesschen
D. Puchalski, N. Copernicus University
E. Gogus, Sabancı University
T. Guver, Istanbul University
S. Bilir, Istanbul University
T. Ak, Istanbul University
M. M. Hohle, Astrophysical Institute and University Observatory Jena, Schillergaesschen
T. O.B. Schmidt, Astrophysical Institute and University Observatory Jena, Schillergaesschen
R. Errmann, Astrophysical Institute and University Observatory Jena, SchillergaesschenFollow
E.L.N. Jensen, Swarthmore CollegeFollow
D. H. Cohen, Swarthmore CollegeFollow
Laurence A. Marschall, Gettysburg CollegeFollow
G. Saral, Harvard–Smithsonian Center for Astrophysics
I. Bernt, Leibnitz Institut fur Astrophysik Potsdam
E. Derman, Ankara University
C. Galan, N. Copernicus University
R. Neuhauser, Astrophysical Institute and University Observatory Jena, SchillergaesschenFollow

Document Type

Article

Publication Date

4-2014

Department

Physics

Abstract

We present the results of 45 transit observations obtained for the transiting exoplanet HATP- 32b. The transits have been observed using several telescopes mainly throughout the YETI (Young Exoplanet Transit Initiative) network. In 25 cases, complete transit light curves with a timing precision better than 1.4 min have been obtained. These light curves have been used to refine the system properties, namely inclination i, planet-to-star radius ratio Rp/Rs, and the ratio between the semimajor axis and the stellar radius a/Rs. First analyses by Hartman et al. suggests the existence of a second planet in the system, thus we tried to find an additional body using the transit timing variation (TTV) technique. Taking also the literature data points into account, we can explain all mid-transit times by refining the linear ephemeris by 21 ms. Thus, we can exclude TTV amplitudes of more than ∼1.5min.

Required Publisher's Statement

Original version is available from the publisher at: http://mnras.oxfordjournals.org/content/441/1/304

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