caa a22 4500 445863358 CHVBK 20180317145450.0 cr unu---uuuuu 170323e20111001xx s 000 0 eng 10.1007/s10569-011-9363-1 doi (NATIONALLICENCE)springer-10.1007/s10569-011-9363-1 On the detection of (habitable) super-Earths around low-mass stars using Kepler and transit timing variation method [Elektronische Daten] [Nader Haghighipour, Sabrina Kirste] We present the results of an extensive study of the detectability of Earth-sized planets and super-Earths in the habitable zones of cool and low-mass stars using transit timing variation method. We have considered a system consisting of a star, a transiting giant planet, and a terrestrial-class perturber, and calculated TTVs for different values of the parameters of the system. To identify ranges of the parameters for which these variations would be detectable by Kepler, we considered the analysis presented by Ford etal. (Transit timing observations from Kepler: I. Statistical analysis of the first four months. ArXiv:1102.0544, 2011) and assumed that a peak-to-peak variation of 20 s would be within the range of the photometric sensitivity of this telescope. We carried out simulations for resonant and non-resonant orbits, and identified ranges of the semimajor axes and eccentricities of the transiting and perturbing bodies for which an Earth-sized planet or a super-Earth in the habitable zone of a low-mass star would produce such TTVs. Results of our simulations indicate that in general, outer perturbers near first- and second-order resonances show a higher prospect for detection. Inner perturbers are potentially detectable only when near 1:2 and 1:3 mean-motion resonances. For a typical M star with a Jupiter-mass transiting planet, for instance, an Earth-mass perturber in the habitable zone can produce detectable TTVs when the orbit of the transiting planet is between 15 and 80 days. We present the details of our simulations and discuss the implication of the results for the detection of terrestrial planets around different low-mass stars. Springer Science+Business Media B.V., 2011 Planetary systems: Detection nationallicence Detection techniques nationallicence Methods: Numerical simulations nationallicence TTV nationallicence Resonant orbits nationallicence Haghighipour Nader Institute for Astronomy and NASA Astrobiology Institute, University of Hawaii, 96825, Honolulu, HI, USA aut Kirste Sabrina Zentrum für Astronomie und Astrophysik (ZAA), Technische Universität Berlin, 10623, Berlin, Germany aut Celestial Mechanics and Dynamical Astronomy Springer Netherlands 111/1-2(2011-10-01), 267-284 0923-2958 111:1-2<267 2011 111 10569 https://doi.org/10.1007/s10569-011-9363-1 text/html Onlinezugriff via DOI 1 research-article jats NATIONALLICENCE 856 40 https://doi.org/10.1007/s10569-011-9363-1 text/html Onlinezugriff via DOI NATIONALLICENCE 700 1- Haghighipour Nader Institute for Astronomy and NASA Astrobiology Institute, University of Hawaii, 96825, Honolulu, HI, USA aut NATIONALLICENCE 700 1- Kirste Sabrina Zentrum für Astronomie und Astrophysik (ZAA), Technische Universität Berlin, 10623, Berlin, Germany aut NATIONALLICENCE 773 0- Celestial Mechanics and Dynamical Astronomy Springer Netherlands 111/1-2(2011-10-01), 267-284 0923-2958 111:1-2<267 2011 111 10569 Metadata rights reserved Springer special CC-BY-NC licence nationallicence BK010053 XK010053 XK010000 NATIONALLICENCE NATIONALLICENCE NL-springer