2 research outputs found
Probing Micro-quasars with TeV Neutrinos
The jets associated with Galactic micro-quasars are believed to be ejected by
accreting stellar mass black-holes or neutron stars. We show that if the energy
content of the jets in the transient sources is dominated by electron-proton
plasma, then a several hour outburst of 1--100 TeV neutrinos produced by photo-
meson interactions should precede the radio flares associated with major
ejection events. Several neutrinos may be detected during a single outburst by
a 1km^2 detector, thereby providing a powerful probe of micro-quasars jet
physics.Comment: Accepted to PRL. More detailed discussion of particle acceleratio
External shock model for the large-scale, relativistic X-ray jets from the microquasar XTE J1550-564
Large-scale, decelerating, relativistic X-ray jets due to material ejected
from the black-hole candidate X-ray transient and microquasar XTE J1550-564 has
been recently discovered with Chandra by Corbel et al. (2002). We find that the
dynamical evolution of the eastern jet at the late time is consistent with the
well-known Sedov evolutionary phase. A trans-relativistic external shock
dynamic model by analogy with the evolution of gamma-ray burst remnants, is
shown to be able to fit the observation data reasonably well. The inferred
interstellar medium density around the source is well below the canonical value
. We find that the emission from the continuously shocked
interstellar medium (forward shock region) decays too slowly to be a viable
mechanism for the eastern X-ray jet. However, the rapidly fading X-ray emission
can be interpreted as synchrotron radiation from the non-thermal electrons in
the adiabatically expanding ejecta. These electrons were accelerated by the
reverse shock (moving back into the ejecta) which becomes important when the
inertia of the swept external matter leads to an appreciable slowing down of
the original ejecta. To ensure the dominance of the emission from the shocked
ejecta over that from the forward shock region during the period of the
observations, the magnetic field and electron energy fractions in the forward
shock region must be far below equipartition. Future continuous, follow-up
multi-wavelength observations of new ejection events from microquasars up to
the significant deceleration phase should provide more valuable insight into
the nature of the interaction between the jets and external medium.Comment: Accepted for publication in ApJ, minor changes; 11 pages, including 5
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