Caracterización espectroscópica del campo magnético de estrellas tipo A y G a partir del método de auto correlación

Abstract

This paper shows the results of a stellar spectroscopy project developed at the Astronomical Observatory of the Universidad de los Andes. The project consists of the study of stellar spectra and the application of a novel technique that uses the spectrum autocorrelation method to measure the average widening of the absorption lines caused by the magnetic field. Spectroscopy is an analysis technique that allows you to study the information contained in the radiation of the stars. Some data that can be determined are the chemical composition, the surface temperature from the black body model, the radial velocity by Doppler effect, in addition to the magnetic field by Zeeman effect, among many other data. In this particular project, using the Zeeman effect and the novel spectral autocorrelation method (Borra and Deschatelets. 2015), the magnetic fields of at least two Sun-type stars will be studied. The signal autocorrelation method is proven to be effective for measuring the average width of the absorption lines of the stars. However, when performing the respective analysis of results it was shown that the data taken for this work are not optimal due to the amount of instrumental noise and air pollution present in the spectra since they cause a large dispersion between the measured widenings.