RT info:eu-repo/semantics/bachelorThesis
T1 Detección de exoplanetas en sistemas binarios. Desarrollo de la metodología.
A1 Sánchez Sánchez, Victoria
K1 Exoplanetas
K1 Sistemas Binarios
AB Exoplanet detection is a field of science to which many resources are currently being allocated. The firstexoplanet was discovered was in 1992 and orbited the pulsar PSR B1257 + 12 of 6.22 milliseconds.Subsequently two other planets were detected in this system. There are many telescopes destined tosearching for Far Earths, such as the Very Large Telescope, in Chile, the 3.6 meter telescope with theHARPS spectrograph, also in Chile, the Keck and Gemini observatories in Hawaii, etc. Among the missionscarried out in this field are the WASP, TrES (with telescopes in Tenerife, Arizona and California) and themissions of Kepler and its K2 extension. To detect these celestial bodies, several methods that require veryprecise instrumentation are used. The direct image method is very limited since it is no useful at greatdistances and the difficulty of capturing the faint brightness of planets in front of the stars which are sobright that they eclipse their surroundings. However, there are several techniques to solve these problems,such as the use of coronographs to hide the central and brightest part of the stars, thus allowing to observeobjects in the vicinity that were previously imperceptible; and the starshade, structures that are attached tospace telescopes to hide unwanted light before it enters the telescope. Astrometry measures the variation inthe apparent position of the stars in the plane of the sky, being more useful for little massive nearby starsthat house planets with wide orbits. Another method of detection is by measuring the period of pulsars,neutron stars that emit jets of light through the magnetic poles that are detectable when they coincide withthe direction of observation. Any variation in this period will indicate the possible existence of a bodyorbiting the star. The first exoplanet was detected by this method. On the other hand, the phenomenon ofgravitational microlensing is also used, which is difficult to observe since the stars must be aligned with theobserver's direction of vision. One of the most used methods is the calculation of the radial velocity of thestar by Doppler displacement of the absorption lines. This method is commonly used in conjunction withtransits / eclipses to confirm the existence of exoplanets. This technique consists in determining the times inwhich the observed eclipses are produced from the light curve and the times calculated by means of a linearadjustment of the order of the eclipse number versus the observed time. The residue is then calculated,subtracting the observed times with the calculated ones, O-C, for later analysis with the Fourier transform,FFT.In this work a comparison is made between two different methods of analyzing the light curves of twodifferent binaries, KIC 10191056 and KIC 9637299. The first presents a peak in the representation of FFTmodules in both primary eclipses and in the secondary ones with the method of parabolic adjustment of theeclipses. However, they are not visible with the differential flow method of the lowest part of the eclipses.The second binary has a peak in secondary eclipses with both methods but due to the noise it is notpredominantly visible in the primary ones. The results are inconclusive, so if there is evidence of a thirdbody, a complementary method would be required to confirm its existence.
YR 2019
FD 2019
LK http://riull.ull.es/xmlui/handle/915/16255
UL http://riull.ull.es/xmlui/handle/915/16255
LA es
DS Repositorio institucional de la Universidad de La Laguna
RD 29-abr-2024