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Three-dimensional numerical model of the Omega Nebula (M17): simulated thermal X-ray emission

Authors

  • J. Reyes-Iturbide,

    Corresponding author
    1. Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, 04510 México, D. F., México
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  • P. F. Velázquez,

    Corresponding author
    1. Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Apdo. Postal 70-543, D.F. México
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  • M. Rosado,

    Corresponding author
    1. Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70-264, 04510 México, D. F., México
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  • A. Rodríguez-González,

    Corresponding author
    1. Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Apdo. Postal 70-543, D.F. México
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  • R. F. González,

    Corresponding author
    1. Centro de Radioastronomía y Astrofísica Teórica, Universidad Nacional Autónoma de México, Apdo. Postal 3-72 (Xangari), C.P. 58089, Morelia, Michoacán, México
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  • A. Esquivel

    Corresponding author
    1. Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Apdo. Postal 70-543, D.F. México
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E-mail: jreyes@astroscu.unam.mx (JR-I); pablo@nucleares.unam.mx (PFV); margarit@astroscu.unam.mx (MR); ary@nucleares.unam.mx (AR-G); rf.gonzalez@astrosmo.unam.mx (RFG); esquivel@nucleares.unam.mx (AE)

ABSTRACT

We present 3D hydrodynamical simulations of the superbubble M17, also known as the Omega Nebula, carried out with the adaptive grid code yguazú-a, which includes radiative cooling. The superbubble is modelled considering the winds of 11 individual stars from the open cluster inside the nebula (NGC 6618), for which there are estimates of the mass-loss rates and terminal velocities based on their spectral types. These stars are located inside a dense interstellar medium, and they are bounded by two dense molecular clouds. We carried out three numerical models of this scenario, considering different line-of-sight positions of the stars (the position in the plane of the sky is known, thus fixed). Synthetic thermal X-ray emission maps are calculated from the numerical models and compared with ROSAT observations of this astrophysical object. Our models successfully reproduce both the observed X-ray morphology and the total X-ray luminosity, without taking into account the thermal conduction effects.

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