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SS433: The Microquasar Link with ULXS?

Published online by Cambridge University Press:  22 February 2018

P. A. Charles
Affiliation:
University of Southampton, Southampton, UK
A. D. Barnes
Affiliation:
University of Southampton, Southampton, UK
J. Casares
Affiliation:
Instituto de Astrofísica de Canarias, La Laguna, Spain
J. S. Clark
Affiliation:
University College London, UK
W. I. Clarkson
Affiliation:
University of Southampton, Southampton, UK
E. T. Harlaftis
Affiliation:
National Observatory, Athens, Greece
R. I. Hynes
Affiliation:
University of Texas at Austin, USA
T. R. Marsh
Affiliation:
University of Southampton, Southampton, UK
D. Steeghs
Affiliation:
Harvard-Smithsonian Center for Astrophysics, CambridgeUSA

Abstract

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SS433 is the prototype microquasar in the Galaxy and may even be analogous to the ULX sources if the jets kinetic energy is taken into account. However, in spite of 20 years of study, our constraints on the natur of the binary system are extremely limited as a result of the difficulty of locating spectral features that can reveal the nature and motion of the mass donor. Newly acquired, high resolution blue spectra taken when the (precessing) disc is edge-on suggest that the binary is close to a common-envelope phase, and hence providing kinematic constraints is extremely difficult. Nevertheless, we do find evidence for a massive donor, as expected for the inferred very high mass transfer rate, and we compare SS433's properties with those of Cyg X-3.

Resumen

Resumen

SS433 es el microcuasar prototipo de la Galaxia, y posiblemente incluso análogo a las mentes ULX si se tien en cuenta la energía cinética de los “jets”. Sin embargo y a pesar de 20 años de estudio, nuestras restriccione sobre la naturaleza, del sistema binario son extremadamente grandes debido a la dincultad de localizar rasgo espectrales capaces de revelar la naturaleza y el movimiento del donador de la masa. Los espectros azules de alts resolución recientemente obtenidos cuando el disco (en precesión) se encuentra de perfil, sugieren que la binara se halla cerca de la fase de envolvente común, lo cual hace extremadamente difícil obtener las restriccione cinélticas. Sin embargo, encontramos evidencia de un donador masivo como era de esperar para la muy alts tasa de transferencia de masa inferida y comparamos las propiedades de SS433 con las de Cyg X3.

Type
The Contributed Papers
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

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