Spin effects in processes with the participation of high-energy particles in a magnetic field

1984 ◽  
Vol 27 (7) ◽  
pp. 550-553
Author(s):  
V. G. Bagrov ◽  
V. Ch. Zhukovskii ◽  
I. M. Ternov ◽  
V. R. Khalilov
Keyword(s):  
Magnetic Field ◽  
High Energy ◽  
Spin Effects ◽  
High Energy Particles

scholarly journals Magnetized Black Holes: Ionized Keplerian Disks and Acceleration of Ultra-High Energy Particles

Proceedings ◽  
2019 ◽  
Vol 17 (1) ◽  
pp. 13 ◽  
Author(s):  
Zdeněk Stuchlík ◽  
Martin Kološ ◽  
Arman Tursunov
Keyword(s):  
Magnetic Field ◽  
Black Holes ◽  
Magnetic Fields ◽  
High Energy ◽  
Weak Magnetic Fields ◽  
Motion Transformation ◽  
Penrose Process ◽  
Field Lines ◽  
High Energy Particles ◽  
Quasiperiodic Oscillations

Properties of charged particle motion in the field of magnetized black holes (BHs) imply four possible regimes of behavior of ionized Keplerian disks: survival in regular epicyclic motion, transformation into chaotic toroidal state, destruction due to fall into the BHs, destruction due to escape along magnetic field lines (escape to infinity for disks orbiting Kerr BHs). The regime of the epicyclic motion influenced by very weak magnetic fields can be related to the observed high-frequency quasiperiodic oscillations. In the case of very strong magnetic fields particles escaping to infinity could form UHECR due to extremely efficient magnetic Penrose process – protons with energy E > 10 21 eV can be accelerated by supermassive black holes with M ∼ 10 10 M ⊙ immersed in magnetic field with B ∼ 10 4 Gs.

Focusing of high-energy particles by a plasma current lens controlled by an external magnetic field

2000 ◽  
Vol 26 (4) ◽  
pp. 351-355
Author(s):  
V. N. Belan ◽  
V. I. Butenko ◽  
A. M. Egorov ◽  
B. I. Ivanov ◽  
V. A. Kiselev ◽  
...  
Keyword(s):  
Magnetic Field ◽  
External Magnetic Field ◽  
High Energy ◽  
Plasma Current ◽  
High Energy Particles

scholarly journals Influence of Cosmic Repulsion and Magnetic Fields on Accretion Disks Rotating around Kerr Black Holes

Universe ◽  
2020 ◽  
Vol 6 (2) ◽  
pp. 26 ◽  
Author(s):  
Zdeněk Stuchlík ◽  
Martin Kološ ◽  
Jiří Kovář ◽  
Petr Slaný ◽  
Arman Tursunov
Keyword(s):  
Magnetic Field ◽  
Black Holes ◽  
Magnetic Fields ◽  
Accretion Disks ◽  
Vacuum Energy ◽  
High Energy ◽  
Supermassive Black Holes ◽  
Ultra High Energy ◽  
Thin And Thick Disks ◽  
High Energy Particles

We present a review of the influence of cosmic repulsion and external magnetic fields on accretion disks rotating around rotating black holes and on jets associated with these rotating configurations. We consider both geometrically thin and thick disks. We show that the vacuum energy represented by the relic cosmological constant strongly limits extension of the accretion disks that is for supermassive black holes comparable to extension of largest galaxies, and supports collimation of jets at large distances from the black hole. We further demonstrate that an external magnetic field crucially influences the fate of ionized Keplerian disks causing creation of winds and jets, enabling simultaneously acceleration of ultra-high energy particles with energy up to 10 21 eV around supermassive black holes with M ∼ 10 10 M ⊙ surrounded by sufficiently strong magnetic field with B ∼ 10 4 G. We also show that the external magnetic fields enable existence of “levitating” off-equatorial clouds or tori, along with the standard equatorial toroidal structures, if these carry a non-vanishing, appropriately distributed electric charge.

scholarly journals Cosmic ray interactions in the solar atmosphere

2019 ◽  
Vol 491 (4) ◽  
pp. 4852-4856 ◽  
Author(s):  
Hugh S Hudson ◽  
Alec MacKinnon ◽  
Mikolaj Szydlarski ◽  
Mats Carlsson
Keyword(s):  
Magnetic Field ◽  
Open Field ◽  
Solar Atmosphere ◽  
Cosmic Ray ◽  
High Energy ◽  
Emission Anisotropy ◽  
Flux Tubes ◽  
Wide Range ◽  
High Energy Particles ◽  
The Magnetic Field

ABSTRACT High-energy particles enter the solar atmosphere from Galactic or solar coronal sources, and produce ‘albedo’ emission from the quiet Sun that is now observable across a wide range of photon energies. The interaction of high-energy particles in a stellar atmosphere depends essentially upon the joint variation of the magnetic field and plasma density, which heretofore has been characterized parametrically as P ∝ Bα with P the gas pressure and B the magnitude of the magnetic field. We re-examine that parametrization by using a self-consistent 3D MHD model (Bifrost) and show that this relationship tends to P ∝ B3.5 ± 0.1 based on the visible portions of the sample of open-field flux tubes in such a model, but with large variations from point to point. This scatter corresponds to the strong meandering of the open-field flux tubes in the lower atmosphere, which will have a strong effect on the prediction of the emission anisotropy (limb brightening). The simulations show that much of the open flux in coronal holes originates in weak-field regions within the granular pattern of the convective motions seen in the simulations.

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