A física do processo de detecção de exoplanetas através da ciência de dados

Abstract

In this work, we discuss the physics behind the most successful exoplanet detection method to date. The planetary transit method. For, the time series of the flow of the star Kepler69 that observes, along the time series of the analyzed flow, we observe along the Kepler light. Using data science techniques for loading, processing, and manipulating the data and using Kepler's high-precision photometry together with the uncertainties associated with its records, we detected two sets of transit signals in the star's flux temporal. For the interior of the planet, kepler-69b, we calculate a radius of 2.21 R⊕ an orbital period of 13.72 days, and a semi-major axis orbit of 0.10 au. The planet, Kepler-69c, presents the stars of being a Super Earth with a radius of 1.87 R⊕, host 242.47 days to complete a revolution around its star and with a view that has a greater than 0.71 au. We also discuss questions about the habitability of these two planets. Kepler-69b is located very close to its star and therefore outside its Habitable Zone. If we assume an Earth-like albedo, Kepler-69c would have an equilibrium temperature of about 28 K. Which puts this planet very close to its star's habitable zone. This Earth-like planet, orbiting a star similar to our Sun in a region close to its habitable zone, represents an important step in the search for planets similar to our home and that may meet the necessary conditions for the emergence and development of life. All the results obtained in this work are compared with the values published in the first article that confirmed these two exoplanets.