Dynamics of charged particles near a black hole in a magnetic field

We therefore down- sampled the NACO data into 100 bins with equal path lengths along the projected orbit (Fig. 4, middle) and gave these data in addition a lower weight of

Likewise, the optical and NIR spectrum is well described by the thermal emission from the viscous accretion disk, with an excess due to the synchrotron emission from the jet,

We used the TAROT network of telescopes to search for the electromagnetic counterparts of GW150914, GW170104 and GW170814, which were reported to originate from binary black hole

Our analysis takes into account inverse Compton scattering and pair creation via the interaction of pairs and gamma rays with an ambient radi- ation field, assumed to be emitted by

For the entire do- main at the time of best depiction of a stratiform region, the areal coverage of positive reflectivity evidenced very differ- ent trends compared to the

A strong magnetic field around the supermassive black hole at the centre of the GalaxyR. Kramer,

general form of the potential relief (or in the presence of a magnetic field) the particle overcoming the saddle point with small kinetic energy will not come back. So,

The six parameters describing the Kepler orbit (a, e, i, ω, Ω , and t 0 ), the distance, and the central mass, and the five coor- dinates describing the position on the sky and