Resumen:

It has been proposed that microquasars may contribute significantly to the galactic CR population, because their non-thermal emission indicates the existence of efficient particle acceleration mechanisms in their jets. Relativistic hadronic content has been observed in some jets, such as those of the microquasar SS 433. In these cases, the production of relativistic neutrons is an inescapable consequence of hadronic interactions. Given that neutrons are not magnetically confined, they escape from the jet and decay, providing a way for charged particles to escape the system, becoming CRs. In this poster we will show the predictions of our model on neutron-driven CR production applied to SS 433, which is a microquasar accreting in a super-Eddington regime, with highly collimated and powerful jets, which renders this source as an excellent candidate for high CR prodution, according to previous results. We will show our preliminary results on the possible scenarios that could explain the observed non-thermal emission of SS 433, the properties of the CRs produced by neutron escape, and discuss the observability of their emission in the surrounding environment of the microquasar.

Resumen:

The origin of stellar explosions associated with long-duration gamma ray bursts (GRB SNe) is a very interesting open topic in stellar astrophysics of massive stars. In all cases, these supernovae (SNe) were classified as type Ic, that is hydrogen- and helium-deficient, showing broad lines in their spectra. This characteristic is indicative of high velocities and energies, and the objects are referred to as SNe Ic-BL. However, there is a number of SNe Ic-BL that have not a GRB observed, which leads to the question of whether it is due to a physical difference or to an observational bias. The aim of this work is to analyze in depth this association and to identify the properties that represent these objects. To this end, we have re-analyzed a sample of GRB SNe previously modeled by our group. The main reason for doing this is that our previous studies used bolometric luminosities calculated using different methods, which prevents comparisons between the objects. Therefore, we have homogenized the calculation method and included new objects to our sample. Then, we modeled the objects using a hydrodynamic code and derived its physical parameters. To conclude, we have compared our results with those obtained for stripped-envelope SNe and SNe Ic- BL that have not been associated to GRB available in the literature. Our findings indicate that more massive progenitor with larger compact remnants consistent with black hole formation are required to reproduce the observations for our sample of GRB SNe.

Resumen:

High energy astronomy constitutes a fundamental field of study in astrophysics, which is in charge of the study of astroparticles, such as gamma rays, which originate in the natural sources of the universe, through the interaction of cosmic radiation with the natural particle accelerator that the cosmos possesses. High-energy gamma rays in the teraelectronvolt (TeV) range are an astrophysical phenomenon of great interest that provide a unique look at the most violent and energetic events in the universe. These events occur in various astronomical objects, such as active galactic nuclei, supernova remnants, pulsars, among others, generating processes such as the collision of particles at high speeds, the acceleration of particles in intense magnetic fields, or the disintegration of subatomic particles. The detection and study of these astroparticles is a technical challenge due to their high energy and low detection rate. However, thanks to advances in instrumentation and observing techniques, such as the air and water Cherenkov telescopes, precise measurements and detailed information on these emissions have been achieved. This is a unique window to study the most energetic and extreme events in the universe.