Speakers
Description
Compact stars (white dwarfs and neutron stars) possess strong magnetic fields that affect their micro and macrophysics. In recent years, several theoretical models of magnetized compact objects have been developed, considering different approximations and assumptions about the geometry and intensity of the stellar magnetic field. Such suppositions reflect on the resulting structure equations, i.e., the solutions of Einstein's field equations used to compute the star's observables. Consequently, many of these models differ in their predictions about the properties of magnetized compact objects. Our goal here is to explore to what extent the effects of the magnetic field on the observables depend on the model used to compute them. To do so, we first compare the predictions of several sets of structure equations, trying to get an insight into their differences. Later, we perform a deeper study for two macroscopic models of axisymmetric non-rotating stars under the action of a uniform and constant magnetic field. We computed the macroscopic properties of magnetized white dwarfs, strange stars, and Bose-Einstein condensate stars given by each of these two models and found that their predictions are consistent as long as they are used with the same equation of state, so that the influence of the magnetic field in the observables mainly depends on the microscopic description of the star. However, there are features that appear to be ruled by the geometry of the magnetic field and the approximations taken to obtain the structure equations. Hence, we propose some strategies to discern between both possibilities.
