My theses

Low-mass eclipsing binary systems frequently display larger radii and lower effective temperatures than standard theoretical stellar models predict for single stars of equal mass. Because these faint systems are difficult to detect, detailed observational analyses are essential to refine current stellar evolutionary models.

This thesis presents a comprehensive photometric and spectroscopic study of the low-mass detached eclipsing binary system ASAS J052919-1617.3. Using optical observations (V, R, I filters) from the IAC80 telescope and spectroscopy from the NOT and INT telescopes, we established the first detailed physical and orbital parameters for the system using PHOEBE. To process the data, automatic Python pipelines were developed for reduction, astrometry, calibration, and adaptive differential aperture photometry. The analysis explicitly accounted for a nearby contaminating star located 3.21″ away, as well as interstellar reddening and distance measurements derived from Gaia DR3.

This work presents the photometric study of two eclipsing binary systems, 2MASS J01074282+4845188 and ASAS J052919-1617.3, using observations obtained with the IAC80 telescope at the Teide Observatory. The study covers the complete observational and data-analysis process, from planning and CCD image acquisition to data reduction, astrometry, and differential photometry.

Using observations in the Johnson–Bessell V, R, and I filters, the primary eclipse times were determined and used to calculate the orbital periods of both systems. The resulting ephemerides allowed the construction and analysis of their light curves. The study also identifies a contaminating source affecting the observations of ASAS J052919-1617.3 and provides evidence supporting the classification of 2MASS J01074282+4845188 as a cataclysmic eclipsing binary, likely involving a white dwarf, a red dwarf, and an accretion disk.