Collimated outflows of particles and radiation produced in astrophysical explosions like supernovae.Relativistic jets are narrow, powerful beams of plasma and radiation that are ejected from the vicinity of compact objects, such as black holes and neutron stars, at speeds close to the speed of light. They are observed across the universe, from supermassive black holes at the centers of galaxies to stellar-mass black holes in binary systems and even from the remnants of supernova explosions. The seed definition highlights their role in astrophysical explosions, where they can punch through the expanding debris of a dying star, as seen in the title 'Звёздные взрывы шлют нам частицы, но не все сразу'.
Jets were first observed in the early 20th century in the galaxy M87, but their relativistic nature was recognized much later. The theoretical framework for jet formation from accretion disks was developed in the 1970s and 1980s by theorists like Roger Blandford and Roman Znajek.
The exact mechanism of jet formation is still an active area of research, but the leading theory involves the extraction of rotational energy from a spinning black hole or neutron star via magnetic fields. The accretion disk of infalling matter, threaded by magnetic field lines, acts like a flywheel. Twisted magnetic field lines accelerate plasma along the rotation axis, collimating it into a jet. The jet's particles are accelerated to extreme energies, producing synchrotron radiation and, in some cases, gamma-ray bursts. The title 'Плазменный шар как ключ к магнетарам и быстрым радиовсплескам' suggests that laboratory plasma experiments can simulate aspects of this process.
Relativistic jets are natural particle accelerators, and studying them helps us understand cosmic ray origins. They also play a crucial role in feedback processes that regulate galaxy formation.
The jet from the supermassive black hole in M87 extends for thousands of light-years, far beyond the galaxy's visible extent.
| \lambda | variable | mean free path — mean free path metre |
| n | variable | number density of particles — number density per cubic metre |
| \sigma | variable | collision cross-section — cross section square metre |










