Variações espaciais de propriedades físicas em Puppis A

• Ano de defesa: 2009
• Autor(a) principal: Melnik, Igor Antonio Cancela
• Tipo de documento: Dissertação
• Tipo de acesso: Acesso aberto
• Idioma: por
• Instituição de defesa: Universidade Federal de Santa Maria; BR; Física; UFSM; Programa de Pós-Graduação em Física
• Palavras-chave em Português: Física; Astronomia; Supernovas; CNPQ::CIENCIAS EXATAS E DA TERRA::FISICA
• Link de acesso: http://repositorio.ufsm.br/handle/1/9197

The current work presents some physical proprieties from a region of the galactic supernova remnant Puppis A. For that, long slit spectrophotometric data were obtained in distinct positions. The data were obtained in 14 distinct positions in the direction North-South, and the distance among slit positions was 5′′. The spectra were obtained by using the Cassegrain spectrograph attached to 1.60 m telescope of the Laborat´orio Nacional de Astrof´ısica, MG, and covered the range between 6000 and 7000 °A. In this range, it was possible to measure the line Hα and the line ratio [S ii] λ6516/λ6531, which was used to determine the electron density. Unidimensionals spectra were extracted by each bidimensional spectrum with sectors of size 2.3′′. Through the unidimensional spectra line mensures, maps of Hα flux, Hα width at half maximum, electron density and radial velocity were buildt. The maps have the same resolution of 2.3′′×5′′. Emission lines with two components were observed, and the maps of the physical proprieties associated with each of them were built. The mean difference between the radial velocity of these components is 214 km s−1. The mapped region presents an irregular density distribution around 887 +347 −247 cm−3. The radial velocity map revealed two different structures. One structure presented positive values of radial velocity and the other presented negative values of radial velocity. This structure have higher electron density than the structure with positive values of radial velocity. The density difference between these structures can be interpreted as an evidence of an interaction between the remnant and a molecular cloud. The mapped region presented a mean velocity dispersion of ≈ 18 km s−1, and the radial velocity values varied from -290 km s−1 to 260 km s−1. The mass of the remnant was estimated between 1.2 M⊙ and 37.2 M⊙.