| Texto completo | |
| Autor(es): |
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]
Número total de Autores: 6
|
| Afiliação do(s) autor(es): | [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
Número total de Afiliações: 7
|
| Tipo de documento: | Artigo Científico |
| Fonte: | ASTROPHYSICAL JOURNAL; v. 908, n. 2 FEB 2021. |
| Citações Web of Science: | 0 |
| Resumo | |
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) | |
| Processo FAPESP: | 19/03301-8 - Observação e modelagem de regiões ativas solares e estelares em ondas rádio mm/sub-mm |
| Beneficiário: | Caius Lucius Selhorst |
| Modalidade de apoio: | Auxílio à Pesquisa - Regular |
| Processo FAPESP: | 13/10559-5 - Investigação de fenômenos de altas energias e plasmas astrofísicos: teoria, simulações numéricas, observações e desenvolvimento de instrumentação para o Cherenkov Telescope Array (CTA) |
| Beneficiário: | Elisabete Maria de Gouveia Dal Pino |
| Modalidade de apoio: | Auxílio à Pesquisa - Projetos Especiais |
| Processo FAPESP: | 16/12320-8 - Estudo numérico de reconexão magnética ao redor de buracos negros |
| Beneficiário: | Luis Henrique Sinki Kadowaki |
| Modalidade de apoio: | Bolsas no Brasil - Pós-Doutorado |
| Processo FAPESP: | 09/54006-4 - Um cluster de computadores para o Departamento de Astronomia do IAG-USP e para o Núcleo de Astrofísica da UNICSUL |
| Beneficiário: | Elisabete Maria de Gouveia Dal Pino |
| Modalidade de apoio: | Auxílio à Pesquisa - Programa Equipamentos Multiusuários |