One of the most successful approaches for the detection of exoplanets is the so called transit method: A star's brightness is continuously measured over time by a powerful telescope. If one or multiple planets orbit this star the recorded luminosity of the star will exhibit periodically recurring dips due to the transits of the planet in front of the telescope's lense – an effect comparable to that of an eclipse. Given how small planets are compared to stars the transit signals are known to be very weak.
The stars included in this file all have known exoplanets with the following periods:
Kepler 1871056: 2 planets with orbital periods of 40.8 and 140.1 days
Kepler 2307415: 2 planets with orbital periods of 4.61 and 12.12 days
Kepler 3102384: 2 planets with orbital periods of 10.57 and 523.9 days
Kepler 3231341: 4 planets with orbital periods of 4.24, 8.15, 12.33, and 19.00 days
Kepler 3447722: 3 planets with orbital periods of 10.30, 16.09, and 35.68 days
Kepler 4139816: 4 planets with orbital periods of 3.34, 7.82, 20.06, and 46.18 days
Kepler 10965588: 1 planet with orbital period of 62.89 days
More information about the exoplanets above and more data can be found at
This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.
A list of seven dataframes named "Kepler1871056", "Kepler2307415", "Kepler3102384", "Kepler3231341", "Kepler3447722", "Kepler4139816", and "Kepler10965588". Each dataframe consists of two columns called "Brightness" and "Day", containing measurements of a star's brightness and the measurement's timestamp respectively.
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