| Texto completo | |
| Autor(es): |
Kadowaki, Luis H. S.
[1]
;
de Gouveia Dal Pino, Elisabete M.
[1]
;
Medina-Torrejon, Tania E.
[2]
;
Mizuno, Yosuke
[3, 4, 5]
;
Kushwaha, Pankaj
[6]
Número total de Autores: 5
|
| Afiliação do(s) autor(es): | [1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, 1226 Matao St, BR-05508090 Sao Paulo - Brazil
[2] Univ Sao Paulo, Inst Fis, Sao Paulo - Brazil
[3] Shanghai Jiao Tong Univ, Sch Phys & Astron, Shanghai 200240 - Peoples R China
[4] Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shanghai 200240 - Peoples R China
[5] Goethe Univ, Inst Theoret Phys, D-60438 Frankfurt - Germany
[6] Aryabhatta Res Inst Observ Sci ARIES, Manora Peak 263001, Nainital - India
Número total de Afiliações: 6
|
| Tipo de documento: | Artigo Científico |
| Fonte: | ASTROPHYSICAL JOURNAL; v. 912, n. 2 MAY 2021. |
| Citações Web of Science: | 0 |
| Resumo | |
The ubiquitous relativistic jet phenomena associated with black holes play a major role in high and very-high-energy (VHE) astrophysics. In particular, observations have demonstrated that blazars show VHE emission with time variability from days to minutes (in the gigaelectronvolt and teraelectronvolt bands), implying very compact emission regions. The real mechanism of the particle acceleration process responsible for this emission is still being debated, but magnetic reconnection has lately been discussed as a strong potential candidate. In this work, we present the results of three-dimensional special relativistic magnetohydrodynamic simulations of the development of reconnection events driven by turbulence induced by current-driven kink instability along a relativistic jet. We have performed a systematic identification of all reconnection regions in the system, characterizing their local magnetic field topology and quantifying the reconnection rates. We obtained average rates of 0.051 +/- 0.026 (in units of Alfven speed), which are comparable to the predictions of the theory of turbulence-induced fast reconnection. A detailed statistical analysis also demonstrated that the fast reconnection events follow a log-normal distribution, which is a signature of its turbulent origin. To probe the robustness of our method, we have applied our results to the blazar Mrk 421. Building a synthetic light curve from the integrated magnetic reconnection power, we evaluated the time variability from a power spectral density analysis, obtaining good agreement with observations in the gigaelectronvolt band. This suggests that turbulent fast magnetic reconnection can be a possible process behind the high-energy emission variability phenomena observed in blazars. (AU) | |
| 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 |
| 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 |