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En el presente trabajo, utilizando una generalización del potencial de Miyamoto-Nagai, se ajustan las curvas de rotación observadas de tres galaxias espirales a las velocidades circulares analiticas. Los datos observacionales se tomaron de un conjunto de imágenes de línea de 21 centímetros (o línea HI) obtenidos con el Westerbork Synthesis Radio Telescope (WSRT), para tres galaxias particulares en el grupo de la Ursa Major: NGC 3726, NGC 3877 y NGC 4010. Seguidamente, se analiza la dinámica del sistema en términos del método de secciones de Poincaré, encontrando que para valores grandes del momento angular de la partícula de prueba o valores bajos su energía total, la din´amica es principalmente regular, mientras que en los casos opuestos, la dinámica es principalmente ca´otica. Nuestro modelo abre la posibilidad de encontrar órbitas caóticas acotadas para estrellas presentes en esas galaxias partículares. © 2019. Acad. Colomb. Cienc. Fis. Nat.
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Derechos de autor 2019 Revista de la Academia Colombiana de Ciencias Exactas, Físicas y Naturales