Speaker
Description
A jet bursting from a high-mass microquasar (HMMQ) behaves just as its scaled-down counterpart bursting from an active galactic nucleus. The jet–wind interaction is conjectured to affect the γ-ray emission. A jet in a HMMQ evolves much faster than its counterpart in an AGN, making the former valuable in studying accretion, eruption, and emission processes around a black hole. In this work, the plasma dynamics and high-energy emission of a relativistic magnetized jet immersed in a stellar wind were studied via simulations. A self-consistent relativistic magnetohydrodynamics (RMHD) model was developed to simulate the plasma evolution by taking into account the interaction among the relativistic jet, stellar wind, and magnetic field. The high-energy emissions out of jet wind interaction via synchrotron radiation and inverse Compton scattering were analyzed by taking a post-processing approach. The values of relevant parameters were estimated from observation data, and the simulated spectrum is similar to that of Cygnus X-1 in the Fermi observation. This model and its simulations results will be very useful in explaining many observed features and predicting more complicated scenarios in the future.
| Participate the oral/poster presentation award competition | No |
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