LS I+61 303: microquasar or not microquasar?
Registro en:
Romero, Gustavo E., Orellana, Mariana D., Okazaki, A. & Owocki, S. (2008). LS I+61 303: microquasar or not microquasar?. World Scientific; International Journal of Modern Physics D; 17; 10; 1875-1881
0218-2718
Autor
Romero, Gustavo E.
Orellana, Mariana D.
Okazaki, A.
Owocki, S.
Institución
Resumen
Fil: Romero, Gustavo E. Instituto Argentino de Radioastronomia; Argentina Fil: Romero, Gustavo E. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Romero, Gustavo E. Comisión de Investigaciones Científicas; Argentina Fil: Orellana, Mariana D. Instituto Argentino de Radioastronomia; Argentina Fil: Orellana, Mariana D. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - La Plata; Argentina Fil: Orellana, Mariana D. Comisión de Investigaciones Científicas; Argentina Fil: Okazaki, A. Hokkai-Gakuen University; Japón Fil: Owocki, S. University of Delaware; Estados Unidos true LS I +61 303 is a puzzling object detected from radio up to high-energy gamma-rays. Variability has recently been observed in its high-energy emission. The object is a binary system, with a compact object and a Be star as primary. The nature of the secondary and the origin of the gamma-ray emission are not clearly established at present. Recent VLBA radio data have been used to claim that the system is a Be/neutron star colliding wind binary, instead of a microquasar. We review the main views on the nature of LS I +61 303 and present results of 3D SPH simulations that can shed some light on the nature of the system. Our results support an accretion powered source, compatible with a microquasar interpretation.