| Full text | |
| Author(s): |
Medina-Torrejon, Tania E.
[1]
;
de Gouveia Dal Pino, Elisabete M.
[2]
;
Kadowaki, Luis H. S.
[2]
;
Kowal, Grzegorz
[3]
;
Singh, Chandra B.
[4]
;
Mizuno, Yosuke
[5, 6, 7]
Total Authors: 6
|
| Affiliation: | [1] Univ Sao Paulo, Inst Fis, Sao Paulo - Brazil
[2] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, 1226 Matao St, BR-05508090 Sao Paulo - Brazil
[3] Univ Sao Paulo, Escola Artes Ciencias & Humanidades, Ave Arlindo Bettio, 1000 Vila Guaraciaba, BR-03828000 Sao Paulo - Brazil
[4] Yunnan Univ, South Western Inst Astron Res, Kunming 650500, Yunnan - Peoples R China
[5] Shanghai Jiao Tong Univ, Sch Phys & Astron, Shanghai 200240 - Peoples R China
[6] Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shanghai 200240 - Peoples R China
[7] Goethe Univ, Inst Theoret Phys, D-60438 Frankfurt - Germany
Total Affiliations: 7
|
| Document type: | Journal article |
| Source: | ASTROPHYSICAL JOURNAL; v. 908, n. 2 FEB 2021. |
| Web of Science Citations: | 0 |
| Abstract | |
Particle acceleration in magnetized relativistic jets still puzzles theorists. In this work, we investigate the acceleration of particles injected into a three-dimensional relativistic magnetohydrodynamical jet subject to current-driven kink (CDK) instability. We find that, once turbulence driven by CDK fully develops, achieving a nearly stationary state, the amplitude of excited wiggles along the jet spine attains maximum growth, causing disruption of the magnetic field lines and the formation of several sites of fast reconnection. Low-energy protons injected into the jet at this state experience exponential acceleration, mostly in directions parallel to the local magnetic field, up to maximum energies E similar to 1016 eV for B similar to 0.1 G and E similar to 1018 eV for B similar to 10 G. The Larmor radius of the particles attaining these energies corresponds to the size of the acceleration region (similar to the diameter of the perturbed jet). There is a clear association of the accelerated particles with regions of fast reconnection. In the early nonlinear growth stage of the CDK, when there are no sites of fast reconnection yet, injected particles with initially much larger energy are accelerated by magnetic curvature drift. We have also obtained the acceleration time due to reconnection with a dependence on the particles' energy, t(A) proportional to E-0.1. The energy spectrum of the accelerated particles develops a power-law index p similar to-1.2 in the beginning, in agreement with earlier works. Our results provide a multidimensional framework for exploring this process in real systems and explain their emission patterns, especially at very high energies, and associated neutrino emission recently detected in some blazars. (AU) | |
| FAPESP's process: | 19/03301-8 - Observation and models of solar and stellar active regions at radio wavelengths (mm/sub-mm) |
| Grantee: | Caius Lucius Selhorst |
| Support Opportunities: | Regular Research Grants |
| FAPESP's process: | 13/10559-5 - Investigation of high energy and plasma astrophysics phenomena: theory, numerical simulations, observations, and instrument development for the Cherenkov Telescope Array (CTA) |
| Grantee: | Elisabete Maria de Gouveia Dal Pino |
| Support Opportunities: | Special Projects |
| FAPESP's process: | 16/12320-8 - Numerical study of magnetic reconnection around black hole |
| Grantee: | Luis Henrique Sinki Kadowaki |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |
| FAPESP's process: | 09/54006-4 - A computer cluster for the Astronomy Department of the University of São Paulo Institute of Astronomy, Geophysics and Atmospheric Sciences and for the Cruzeiro do Sul University Astrophysics Center |
| Grantee: | Elisabete Maria de Gouveia Dal Pino |
| Support Opportunities: | Multi-user Equipment Program |