Objeto central compacto como fonte de raios cósmicos

• Ano de defesa: 2023
• Autor(a) principal: Padilha, Luana Natalie
• Tipo de documento: Dissertação
• Tipo de acesso: Acesso aberto
• Idioma: por
• Instituição de defesa: Universidade Tecnológica Federal do Paraná; Curitiba; Brasil; Programa de Pós-Graduação em Física e Astronomia; UTFPR
• Palavras-chave em Português: Aceleradores de partículas; Raios cósmicos; Raios gama; Radiação; Espalhamento (Física); Particle accelerators; Cosmic rays; Gamma rays; Radiation; Scattering (Physics); CNPQ::CIENCIAS EXATAS E DA TERRA::ASTRONOMIA; Física
• Link de acesso: http://repositorio.utfpr.edu.br/jspui/handle/1/30925

The generation of particle energies in the universe is one of the great mysteries of modern science. In recent years, some efforts have been made to identify galactic sources capable of accelerating to the order of PeV and known as PeVatrons. The different morphology of galactic supernova remnants (SNRs) directly correlates with the type of stellar explosion and the existence of a possible central compact object (CCO). CCOs have small radii and intense gravitational fields on their surfaces. Because of these strong and suspended fields with magnetized clouds around them, they are considered possible candidates for cosmic ray production. In August 2002, the XMM-Newton spacecraft performed two of its orbits to the compact object 1E 1207.4-5209 with a total observing time of 257.303 s. The compact X-ray source 1E 1207.4- 5209, classified as a quiet, magnetized, and rapidly rotating neutron star, is in close proximity to the remnant center G296.5+10.0. This association, the compact object 1E 1207.4-5209 and the supernova G296.5+10.0, is located in the constellation Centaurus at an estimated distance of about 2.0 Kpc. In this work, we have determined the transmission of high-energy gammaray emission (E > 100 GeV) through cosmic-ray interference and control of the compact central object 1E 1207.4-5209 and its host SNR G296.5+10.0 by simulation models using GALPROP software. In addition, a contribution to the emission of high-energy gamma rays due to cosmic ray interference by the soft gamma repeater (SGR) J1935+2154 (also known as the first Galactic fast-radio burst) has been determined in a series of papers. and its host SNR G57.2+0.8, using the same CCO methodology. Here we consider the SNR + SGR association as a single source near the Galactic center. The contributions of these associations to the total observed Galactic cosmic ray flux are also calculated, taking into account the manifestation of cosmic rays within the Galaxy with all energy losses and particle reflections. It is suggested that the above configurations can provide a rich scenario for the production of GeV-TeV ranges of cosmic rays up to PeV within the Galaxy.