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project [2013/03/05 21:30]
Gracjan Maciejewski
project [2017/02/21 10:23] (current)
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 +===== STRATEGY =====
 +Timing of transiting exoplanets is expected to provide discoveries of additional, even very low mass bodies in extrasolar systems. In a single-planet system, a transiting planet orbits its host star on a Keplerian orbit. If there is another planet in the system, it interacts gravitationally with the transiting planet what generates deviations from the strictly Keplerian case. These perturbations result in a quasi-periodic signal in an observed-minus-calculated (O-C) diagram of the transiting planet. The TTV method is sensitive to small perturbing masses in orbits near to the low-order mean-motion resonances. Deriving the orbital elements and mass of the perturber from the TTV signal is a difficult inverse problem. Different configurations may generate similar TTV characteristics with an identical dominant periodicity. For a given transiting planet, the TTV signal depends on perturber'​s mass and its orbital elements. Exploring such a multi-dimensional space of parameters is not a trivial task and systematic observations are crucial to finding a correct solution.
 +Data from telescopes located at various longitudes are needed to observe most target'​s transits which are available in an observing season. Thus, we organise multi-site campaigns which engage telescopes in Europe, Asia and America. Our strategy may be summarised as follows:
 +  * Choosing a target sample: the most promising targets are being selected by reanalysis of available literature data. We observe only 2--3 targets in a given season to maximise the efficiency of the project.
 +  * Reconnaissance campaign: an attempt to detect TTV with telescopes smaller than 1 m. If a TTV signal is detected, a provisional hypothesis is put forward. Models, which assume the existence of a perturber in a system and reproduce observed variation of timing residuals, are identified by three-body simulations.
 +  * Follow-up campaign: a photometric follow-up is run with big telescopes (>1 m) to verify and characterise TTV signal. In some cases a spectroscopic follow-up is organised to get more precise radial velocity measurements. If a claimed TTV signal is confirmed, a final hypothesis is elaborated, based on both high-precision photometric and spectroscopic data.
 +  * Direct confirmation:​ attempts to detect transits of a perturbing planet by photometry acquired by large telescopes.
project.txt ยท Last modified: 2017/02/21 10:23 (external edit)
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